Difference between revisions of "Lynds Target Selection"

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My original thoughts on good targets were the following three:
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My original thoughts on good targets were the following three: LDN 470, LDN 1225, LDN 880  (but maybe too diaphanous).  And, at the AAS, you guys also came up with LDN 1340.
−
*LDN 470
+
 
−
*LDN 1225
+
=General information re: lists of targets=
−
*LDN 880  (but maybe too diaphanous)
 
−
And, at the AAS, you guys also came up with
 
−
*LDN 1340
 
  
 
The master list of objects that I worked from is [[lyndslist.txt|here]], courtesy of Babar Ali.  Note that these are all opacity class 5 objects.  Opacity class 5 or higher is what we probably want for Spitzer observations.  None of these have many references in ADS.  '''This is not meant to be a comprehensive list''' by any means, just a place to start.  If you want to instead start with the complete Lynds Dark Nebulae catalog, it's [http://adsabs.harvard.edu/abs/1996yCat.7007....0L here] (the data are linked as "online data" or something similar).
 
The master list of objects that I worked from is [[lyndslist.txt|here]], courtesy of Babar Ali.  Note that these are all opacity class 5 objects.  Opacity class 5 or higher is what we probably want for Spitzer observations.  None of these have many references in ADS.  '''This is not meant to be a comprehensive list''' by any means, just a place to start.  If you want to instead start with the complete Lynds Dark Nebulae catalog, it's [http://adsabs.harvard.edu/abs/1996yCat.7007....0L here] (the data are linked as "online data" or something similar).
  
 
Please post your thoughts and reactions to each of these targets, and any new ones you think are viable candidates for observation.  For example, you might post a gif or jpeg of the POSS image you found, or a summary list of references (e.g., "3 papers besides Lynds, one radio, others submm" or whatever).  Note the syntax I'm using to post comments on LDN 1340 below -- this is a method suggested by the Oil City folks, and I think it works really well to follow the conversation.  See the help page linked from the left (above the search box) for hints on how do this.
 
Please post your thoughts and reactions to each of these targets, and any new ones you think are viable candidates for observation.  For example, you might post a gif or jpeg of the POSS image you found, or a summary list of references (e.g., "3 papers besides Lynds, one radio, others submm" or whatever).  Note the syntax I'm using to post comments on LDN 1340 below -- this is a method suggested by the Oil City folks, and I think it works really well to follow the conversation.  See the help page linked from the left (above the search box) for hints on how do this.
 +
 +
--[[User:Guastella|Guastella]] 20:48, 8 January 2008 (PST)
 +
Here is the article I mentioned in our meeting earlier today. ''(this is the one that looked in radio at optically-selected cores and reported which ones were "empty."'')
 +
 +
THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 123:233È250, 1999 July
 +
(1999. The American Astronomical Society. All rights reserved. Printed in U.S.A.
 +
A CATALOG OF OPTICALLY SELECTED CORES
 +
CHANG WON LEE AND PHILIP C. MYERS
 +
[...]
 +
This didn't format well.  Please let me know if there is a better way to send papers
 +
Thanks
 +
Pete [END]
 +
 +
(--[[User:Rebull|Rebull]] 09:25, 9 January 2008 (PST) he's right, this didn't format well, so I replaced it with a link directly to ADS, from which you can get the complete article - there's no access restrictions on it, and if you go there, you can get the originally formatted PDF or the html.  [http://adsabs.harvard.edu/abs/1999ApJS..123..233L ADS link to the Lee and Myers paper] [END] )
 +
 +
--[[User:Rebull|Rebull]] 13:44, 14 January 2008 (PST) David added some general target selection stuff to the [https://coolwiki.ipac.caltech.edu/index.php/Talk:Lynds_Target_Selection talk page] [END]
 +
 +
--[[User:Rebull|Rebull]] 07:55, 18 January 2008 (PST) [[weeding down a big target list]] - step-by-step, what I did to weed down the full Lynds target list. [END]
 +
 +
=Observing time=
 +
--[[User:Rebull|Rebull]] 13:59, 14 January 2008 (PST) David asked re: time to cover area.
 +
A map I have here that goes about the depth we want covers about 0.6deg x0.6 deg with IRAC takes 1.5 hrs, and more or less the same area takes another 1.4 hrs with MIPS.  3 hrs is probably too much to ask for, especially if you want to ask for more than one cloud.  less than that size, 0.3 deg x 0.3 deg, with IRAC takes 0.4 hrs, and up to 0.7 hrs with MIPS. (i can get clever and try to make that less time, but this is the lowest-energy solution.)  For an irregularly-sized thing like LDN 951, i can get creative and make something other than a square map, but it takes longer for me to design.
 +
so we need to decide if '''(a) we have something really cool we want to completely map, or (b) two smaller things (could be pieces of a large thing) we want to map to compare them.'''
 +
Note that, for example, the object LDN 1340 is more like ~1 degree x ~1 degree, so we'd have to do just a small piece (or two small pieces) of it.
 +
[END]
  
 
=LDN 470=
 
=LDN 470=
 +
 +
[[image:ldn470possred.gif]]  LDN 470 in POSS-red.  image is 0.25 deg on a side. --[[User:Rebull|Rebull]] 14:09, 14 January 2008 (PST)
 +
 +
--[[User:Mcdonald|Mcdonald]] 15:39, 15 January 2008 (PST)  Hi, here is a colored image of LDN 470:
 +
  [[Image:ldn470.jpg]]
  
 
=LDN 1225=
 
=LDN 1225=
 +
 +
[[image:ldn1225possred.gif]]  LDN 1225 in POSS-red.  image is 0.25 deg on a side. --[[User:Rebull|Rebull]] 14:09, 14 January 2008 (PST)
 +
 +
--[[User:Mcdonald|Mcdonald]] 15:44, 15 January 2008 (PST)  Here is a 15 arcmin x 15 arcmin colored image of ldn1225:
 +
  [[Image:ldn1225.jpg]]
  
 
=LDN 880=
 
=LDN 880=
  
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Here is the article I mentioned in our meeting earlier today.
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[[image:ldn880possred.gif |left]]  LDN 880 in POSS-red.  image is 0.25 deg on a side.  Still a little worried that this is too optically thin to make a good Spitzer image.  but maybe we could focus very specifically on the dark thing to the southwest.  
 +
--[[User:Rebull|Rebull]] 14:09, 14 January 2008 (PST)
  
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THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 123:233È250, 1999 July
+
[[image:deepi.png]] [[image:deepr.png]] - LDN 880, about the same scale, in relatively deep I and R from the USNO 1.0m.
−
(1999. The American Astronomical Society. All rights reserved. Printed in U.S.A.
+
--[[User:Rebull|Rebull]] 14:43, 14 January 2008 (PST)
−
A CATALOG OF OPTICALLY SELECTED CORES
 
−
CHANG WON LEE AND PHILIP C. MYERS
 
−
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street,MS 42, Cambridge, MA 02138; cwlee=cfa.harvard.edu, pmyers=cfa.harvard.edu
 
−
Received 1998 October 7; accepted 1999 February 23
 
−
ABSTRACT
 
−
We present a new catalog of 406 dense cores optically selected by using the STScI Digitized Sky
 
−
Survey (DSS). In this catalog 306 cores have neither an embedded young stellar object (EYSO) nor a
 
−
preÈmain-sequence (PMS) star, 94 cores have EYSOs (one core has both an EYSO and a PMS star),
 
−
and six cores have PMS stars only. Our sample of dense cores in the catalog is fairly complete within a
 
−
category of northern Lynds class 5 and 6 clouds and southern Hartley et al. class A clouds, providing a
 
−
database useful for the systematic study of dense cores. Most of the cores listed in the catalog have
 
−
diameters between 0.05 and 0.36 pc with a mean of D0.24 pc. The sizes (D0.33 pc in the mean) of cores
 
−
with EYSOs are found to be usually larger than the sizes (D0.22 pc in the mean) of starless cores. The
 
−
typical mean gas density of the cores is D7]103 cm~3. Most of the cores are more likely elongated
 
−
than spherical (mean aspect ratio : D2.4). The ratio of the number of cores with EYSOs to the number of
 
−
starless cores for our sample is about 0.3, suggesting that the typical lifetime of starless cores is 0.3È1.6
 
−
Myr, about 3 times longer than the duration of the class 0 and class I phases. This lifetime is shorter
 
−
than expected from models of ambipolar di†usion, by factors of 2È44.
 
−
Subject headings : catalogs È ISM: clouds È stars : preÈmain-sequence
 
−
1. INTRODUCTION
 
−
Low-mass stars are generally believed to form through
 
−
the inward gravitational collapse of ““ dense cores ÏÏ with
 
−
density Z a few 104 cm~3, which are expected to form via
 
−
ambipolar di†usion processes (Shu, Adams, & Lizano 1987;
 
−
Ciolek & Mouschovias 1995). However, the knowledge of
 
−
such simple processes in star formation is almost entirely
 
−
theoretical because there is still very little direct observational
 
−
support. It is therefore desirable to conduct
 
−
unbiased systematic surveys of dense cores to search for
 
−
evidence of core evolution and star-forming motion.
 
−
The optical dark cloud catalogs of Lynds (1962), Feitzinger
 
−
& Stu�we (1984), and Hartley et al. (1986, hereafter
 
−
HMSTG), based on visual inspection of optical sky survey
 
−
prints, have provided us the most basic and complete set of
 
−
sources for the study of star-forming regions, although these
 
−
catalogs themselves could not give accurate positions for a
 
−
systematic survey of dense cores because the positions of
 
−
dark regions were determined approximately by eye. Using
 
−
these catalogs has served as a basis for making more accurate
 
−
and detailed catalogs. For the northern hemisphere,
 
−
Myers, Linke, & Benson (1983, hereafter MLB) have collected
 
−
90 small (angular size \5@) opaque spots through
 
−
visual inspection of the Palomar Sky Atlas prints to
 
−
conduct a systematic survey in 13CO, C18O (1È0) lines, and
 
−
later NH (Benson & Myers 1989, hereafter BM). Clemens & Barvai3nis (1988, hereafter CB) have also identiÐed 248
 
−
molecular clouds with optical sizes smaller than 10@ by procedures
 
−
similar to MLBÏs method. For the southern hemisphere,
 
−
Vilas-Boas, Myers, & Fuller (1994) selected 101
 
−
condensations with average optical size less than 7@ and
 
−
visual extinction greater than 2.5 mag from ESO J plates,
 
−
visual extinction maps (Hetem, Sanzovo, & Lepine 1988),
 
−
and the HMSTG catalog to observe them in the 13CO and
 
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C18O (1È0) lines. Bourke, Hyland, & Robinson (1995a) have
 
−
compiled 169 Bok globuleÈlike small (\10@) dark clouds
 
−
from visual inspection of the SERC Schmidt survey J plates
 
−
primarily with the guidance of the HMSTG catalog and
 
−
observed all the cores in the ammonia (1,1) line (Bourke et
 
−
al. 1995b).
 
−
These e†orts resulted in an excellent database for the
 
−
observational study of low-mass star formation. However,
 
−
the samples given in these catalogs were limited to a few
 
−
regions, and many cores are still missing even toward the
 
−
searched area, so these previous studies are not complete.
 
−
Moreover, most opaque positions of the dark clouds in
 
−
these catalogs were determined by eye, so that positions are
 
−
not only very subjective but also not accurate enough for an
 
−
efficient survey in molecular lines.
 
−
Now, through the e†orts of the Space Telescope Science
 
−
Institute (STScI), the Digitized Sky Survey (DSS) data are
 
−
available for us. These data allow us to computerize the
 
−
selection of cores and accurately determine their positions.
 
−
With the guidance of the Lynds (1962) catalog for the northern
 
−
sky and the Hartley et al. (1986) catalog for the southern
 
−
sky, in addition to several reference catalogs that have been
 
−
used for numerous molecular line studies (see ° 2 for
 
−
detailed references), we created a new catalog of dense cores
 
−
using the STScI DSS. Our catalog presents the most complete
 
−
list of optically selected dense cores whose positions
 
−
were accurately measured within a few arcseconds. The
 
−
actual accuracy of positions is dependent only upon the
 
−
procedures for smoothing the data and centering the intensity
 
−
minima of the core.
 
−
In the following section we describe in detail how we
 
−
selected the cores. Then we analyze the statistics of the
 
−
physical parameters of our sample and discuss the implications
 
−
of core statistics for the present standard model
 
−
of isolated star formation. Finally we summarize our results
 
−
in ° 3.
 
−
2. THE CATALOG
 
−
2.1. Selection of Cores
 
−
Our method for the selection of cores is to image an area,
 
−
usually 0¡.5]0¡.5 and occasionally 1¡.0]1¡.0 around a reference
 
−
position, and to make a contour map of optical
 
−
233
 
−
234 LEE & MYERS
 
−
extinction to select the multiple local minimum positions of
 
−
intensity. For guiding reference positions, we used the following:
 
−
BM (NH peaks), Onishi et al. (1996 ; C18O peaks), Codella et al. (19937; NH peaks), Lemme et al. (1996; 3 NHpeaks), and Lynds (1962 ; every Lynds clouds with opacity 53
 
−
and 6) for northern clouds, and Vilas-Boas et al. (1994;
 
−
C18O peaks) and HMSTG (clouds with density class A) for
 
−
southern clouds (Table 1). Digitized data1 were retrieved
 
−
from the STScI DSS using the ““ getimage ÏÏ software
 
−
package provided by STScI. Image processing was conducted
 
−
with the IRAF software package2 (Tody 1993). An
 
−
accurate reading (within error of a few arcseconds) of coordinates
 
−
of local intensity minima in the contour map overlapped
 
−
in the gray image in IRAF was made possible by
 
−
browsing images in World Coordinate Space (Mink 1995)
 
−
with the ““ SAOimage ÏÏÈX11 window based image display
 
−
program (VanHilst 1990). However, the real accuracy of our
 
−
positions was dependent upon the grid size we used to make
 
−
smooth contours and center the intensity minima of the
 
−
core, usually about 15AÈ50A. In order to check the reliability
 
−
of our method, we compared our new positions with peak
 
−
positions of NH maps (with beam resolution of 87A) for 22 cores by BM. T3he di†erence [68@@^10@@ (mean^s.e.m.)]
 
−
between the two positions was found to be smaller than the
 
−
beam resolution of the NH maps, meaning that our method is fairly reliable for3 determining the intensity
 
−
minima positions of new cores.
 
−
Figure 1 shows one example of new core selection using
 
−
the dark cloud, L1622. This example is typical in that
 
−
several distinct intensity minima are obtained for each reference
 
−
position. In total, we examined 250 reference positions
 
−
(Table 1) and identiÐed 406 local maxima of optical extinction
 
−
(Table 2), which we call cores. For all sources, we
 
−
searched the IRAS Point Source Catalog using the ““ riras ÏÏ
 
−
package (D. J.Mink 1998, private communication) to determine
 
−
which sources have embedded IRAS point sources. In
 
−
the search, we assumed the IRAS point source to be an
 
−
““ embedded ÏÏ young stellar object (EYSO) when it satisÐes
 
−
all of the following criteria :
 
−
1. There should be detections in at least two of the four
 
−
IRAS wavelength bands.
 
−
2. The detected Ñuxes (F) should be greater in the longer
 
−
wavelength. However, IRAS point sources with F100km\
 
−
F60km or or were con- , F100km\F25kmsidered to be EYSO, s Fas100kmlo\ngF12akms F60km[
 
−
F25km[F12km.
 
−
3. The projected position of the IRAS source on the sky
 
−
should be enclosed by the contour of the least extinction
 
−
level of core in the optical image.
 
−
1 Images from the northern plates (POSS) were based on photographic
 
−
data of the National Geographic SocietyÈPalomar Geographic Society to
 
−
the California Institute of Technology, and images from the southern
 
−
plates (SERC-J) were based on photographic data obtained using the UK
 
−
Schmidt Telescope. The plates were processed into the present compressed
 
−
digital form with their permission. The UK Schmidt Telescope was operated
 
−
by the Royal Observatory Edinburgh, with funding from the UK
 
−
Science and Engineering Research Council, until 1988 June, and thereafter
 
−
by the Anglo-Australian Observatory. The Digitized Sky Survey was produced
 
−
at the Space Telescope Science Institute under US government grant
 
−
NAGW-2166.
 
−
2 IRAF is distributed by the National Optical Astronomy Observatories,
 
−
which are operated by the Association of Universities for Research
 
−
in Astronomy, Inc., under cooperative agreement with the National
 
−
Science Foundation.
 
−
With these criteria, we searched all cores to determine
 
−
whether there are EYSOs within a box with a size of 2 times
 
−
the geometric mean of the FWHM of a core. The FWHM
 
−
of the core was obtained from an extinction contour map of
 
−
the core as described in the next section. We found 94
 
−
sources with EYSOs and 306 cores without EYSOs. Our
 
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criteria are very similar to those of BMbut di†er from those
 
−
of Beichman et al. (1986) and Wood, Myers, & Daugherty
 
−
(1994) in that ours were designed to preferentially select
 
−
embedded protostars (class 0 and class I YSOs) and therefore
 
−
not to include preÈmain-sequence (PMS) stars. To Ðnd
 
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a possible PMS star, we used color-color diagram criteria in
 
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the 12, 25, and 60 km IRAS bands of Weintraub (1990) :
 
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[2.00\log (l12F12 and /l25 F25)/log (l12/l25)\1.35
 
−
[1.75\log (l25F25 Five /l60 F60)/log (l25/l60)\2.20.
 
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cores were found to have possible PMS stars. We also
 
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searched the catalog of PMS stars by Herbig & Bell (1988)
 
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in which PMS stars were identiÐed by optical spectroscopic
 
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data. From this search two more sources were found to
 
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include PMS stars within their projected extents. Thus we
 
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believe that seven sources may have PMS stars. We note
 
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that one of seven contains EYSO as well.
 
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In summary, of 406 identiÐed cores, 306 were found to
 
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have neither an EYSO nor a PMS star, 94 were found to
 
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have EYSOs (one core has both an EYSO and a PMS star),
 
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and six to have a PMS star only. Henceforth we call the 306
 
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cores with neither an EYSO nor a PMS star ““ starless
 
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cores. ÏÏ In Table 2, column (9), the starless cores are marked
 
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as N and cores with EYSOs as Y, cores with a PMS star are
 
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marked as PM or PM* for a PMS star known by optical
 
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spectroscopy (Herbig & Bell 1988), and cores with both an
 
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EYSO and a PMS star are marked as Y/PM. The IRAS
 
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point sources and the PMS stars believed to be associated
 
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with our optically selected cores are listed in Table 3.
 
−
2.2. Statistics of Physical Parameters of Cores
 
−
In this section we discuss the statistics of the physical
 
−
parameters of cores. Our sample statistics are believed to be
 
−
representative of the core properties since the cores were
 
−
selected from Lynds class 5 and 6 and HMSTGÏs class A,
 
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which, taken together, comprise a nearly complete set of the
 
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densest and the most opaque clouds in the sky.
 
−
We present several physical parameters of the optically
 
−
selected cores in Table 2. The sizes of the major axis (a in
 
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col. [5] of Table 2) and the minor axis (b in col. [6] of Table
 
−
2), and position angle (PA in col. [8] of Table 2) of the
 
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FWHM of the cores were approximately measured by an
 
−
ellipse template, ruler, and protractor. The minus and plus
 
−
signs in column (8) mean clockwise and counterclockwise
 
−
with respect to equatorial north, respectively. The largest
 
−
errors for these parameters are from the uncertainties in the
 
−
selection of the background level of the core that determines
 
−
the size of the FWHM of the core and in the eye Ðtting of
 
−
the ellipse template to the core. The errors obtained by
 
−
repeating measurements are usually within about 10% of
 
−
the size in the size measurement and within about 5¡ in the
 
−
PA measurement. For the sources that are not elliptical in
 
−
shape, their ““ equivalent ÏÏ diameters (R in col. [7] of Table
 
−
2) were measured. The equivalent diameter of a core is
 
−
deÐned as 2](A/n)0.5, where A is the area within the
 
−
FWHM contour of the core. Following are our results and
 
−
discussion on the statistics of these physical parameters.
 
−
TABLE 1
 
−
SEARCHED REFERENCE REGIONS
 
−
Regiona R.A. (1950) Decl. (1950) Referenceb Nc Regiona R.A. (1950) Decl. (1950) Referenceb Nc
 
−
L1291 . . . . . . . . . . . . . . . . 00 39 47.6 61 44 35 Lynds 1 L260 . . . . . . . . . . . . . . . . . 16 44 22.3 [09 30 02 BM 1
 
−
L1333 . . . . . . . . . . . . . . . . 02 21 10.2 75 13 32 Lynds 1 L158* . . . . . . . . . . . . . . . 16 44 42.0 [13 54 03 BM 6
 
−
L1355 . . . . . . . . . . . . . . . . 02 48 41.4 68 43 36 Lynds 1 L204BC* . . . . . . . . . . . . 16 44 51.0 [12 09 00 BM 6
 
−
L1358 . . . . . . . . . . . . . . . . 02 51 00.0 69 10 00 Lynds 2 L191 . . . . . . . . . . . . . . . . . 16 44 59.2 [12 35 31 BM 2
 
−
L1450D . . . . . . . . . . . . . 03 25 18.8 30 53 02 BM 1 L255 . . . . . . . . . . . . . . . . . 16 45 01.9 [09 48 32 Lynds 2
 
−
B5 . . . . . . . . . . . . . . . . . . . . 03 45 16.3 32 44 59 BM 1 L234 . . . . . . . . . . . . . . . . . 16 45 38.0 [10 56 00 BM 3
 
−
CB 17 . . . . . . . . . . . . . . . 04 00 35.0 56 48 00 Le 1 L162 . . . . . . . . . . . . . . . . . 16 46 40.0 [14 04 10 Lynds 2
 
−
L1498 . . . . . . . . . . . . . . . . 04 07 50.0 25 02 13 BM 1 L63 . . . . . . . . . . . . . . . . . . 16 47 21.0 [18 01 00 BM 4
 
−
L1495 . . . . . . . . . . . . . . . . 04 15 18.0 28 25 00 ON 2 L141 . . . . . . . . . . . . . . . . . 16 48 03.1 [15 16 54 Lynds 3
 
−
L1506B . . . . . . . . . . . . . . 04 16 03.9 25 13 01 Lynds 1 L129 . . . . . . . . . . . . . . . . . 16 52 18.4 [16 17 10 Lynds 1
 
−
L1506A . . . . . . . . . . . . . . 04 20 18.0 24 54 00 ON 1 L122 . . . . . . . . . . . . . . . . . 16 52 22.4 [16 42 03 Lynds 1
 
−
L1399 . . . . . . . . . . . . . . . . 04 20 27.0 54 51 00 Lynds 3 L146 . . . . . . . . . . . . . . . . . 16 53 37.0 [15 55 00 Lynds 1
 
−
L1521B . . . . . . . . . . . . . . 04 20 48.0 26 31 40 BM 2 CB 68 . . . . . . . . . . . . . . . 16 53 52.0 [16 00 00 Le 3
 
−
B213-7 . . . . . . . . . . . . . . . 04 22 24.0 26 24 00 ON 1 DC 3504]44 . . . . . . . 16 59 40.9 [34 20 44 HMSTG 1
 
−
B217 . . . . . . . . . . . . . . . . . 04 24 42.5 26 11 13 BM 2 L111 . . . . . . . . . . . . . . . . . 17 11 59.5 [20 27 15 Lynds 1
 
−
L1521 . . . . . . . . . . . . . . . . 04 25 36.0 26 45 00 ON 2 L100 . . . . . . . . . . . . . . . . . 17 13 07.6 [20 54 04 Lynds 1
 
−
L1407 . . . . . . . . . . . . . . . . 04 25 37.6 54 07 35 Lynds 1 L173 . . . . . . . . . . . . . . . . . 17 14 25.4 [18 27 45 Lynds 1
 
−
L1400AK . . . . . . . . . . . 04 25 47.0 54 48 00 BM 4 L1768 . . . . . . . . . . . . . . . 17 17 00.0 [26 49 00 Lynds 2
 
−
L1521E . . . . . . . . . . . . . . 04 26 17.0 26 07 47 BM 1 L1773 . . . . . . . . . . . . . . . 17 18 08.4 [26 50 46 Lynds 1
 
−
L1524 . . . . . . . . . . . . . . . . 04 26 22.0 24 26 30 ON 4 L1774 . . . . . . . . . . . . . . . 17 19 32.1 [27 02 25 Lynds 1
 
−
L1445 . . . . . . . . . . . . . . . . 04 28 28.8 46 31 01 Lynds 1 B68 . . . . . . . . . . . . . . . . . . 17 20 23.0 [23 47 13 BM 3
 
−
L1551S . . . . . . . . . . . . . . 04 28 40.0 18 01 52 BM 2 DC 3463[41 . . . . . . . 17 22 40.3 [42 37 01 HMSTG 1
 
−
B18-2 . . . . . . . . . . . . . . . . 04 29 00.0 24 35 53 ON 1 DC 3479[44 . . . . . . . 17 28 52.7 [41 32 37 HMSTG 1
 
−
TMC 2 . . . . . . . . . . . . . . 04 29 13.0 24 20 14 BM 4 L425 . . . . . . . . . . . . . . . . . 17 44 15.4 [04 34 07 Lynds 1
 
−
L1536B . . . . . . . . . . . . . . 04 29 54.0 22 52 00 ON 2 DC 3475[80 . . . . . . . 17 44 26.1 [43 42 02 HMSTG 1
 
−
L1536A . . . . . . . . . . . . . . 04 30 26.0 22 36 10 BM 1 L392 . . . . . . . . . . . . . . . . . 17 50 24.3 [08 26 43 Lynds 1
 
−
B18-3 . . . . . . . . . . . . . . . . 04 30 53.7 24 05 09 ON 1 L421 . . . . . . . . . . . . . . . . . 17 51 38.9 [05 46 02 Lynds 1
 
−
B18-4 . . . . . . . . . . . . . . . . 04 32 36.0 24 02 00 ON 2 L460 . . . . . . . . . . . . . . . . . 17 55 24.4 [03 46 24 Lynds 1
 
−
L1527 . . . . . . . . . . . . . . . . 04 36 00.0 26 10 00 Lynds 2 L432 . . . . . . . . . . . . . . . . . 17 55 46.2 [05 43 45 Lynds 1
 
−
L1534 . . . . . . . . . . . . . . . . 04 36 31.2 25 35 56 BM 1 L468 . . . . . . . . . . . . . . . . . 17 57 38.0 [03 30 03 Lynds 1
 
−
CB 22 . . . . . . . . . . . . . . . 04 37 25.0 29 48 57 Le 1 L462 . . . . . . . . . . . . . . . . . 18 04 48.0 [04 42 08 Lynds 1
 
−
TMC 1 . . . . . . . . . . . . . . 04 38 19.0 25 45 30 BM 2 L108 . . . . . . . . . . . . . . . . . 18 07 08.0 [28 18 41 Lynds 1
 
−
L1507A . . . . . . . . . . . . . . 04 39 29.0 29 38 07 CO 2 L422 . . . . . . . . . . . . . . . . . 18 09 20.0 [08 04 46 Lynds 1
 
−
L1507B . . . . . . . . . . . . . . 04 39 53.4 29 38 25 Lynds 3 L436-8 . . . . . . . . . . . . . . 18 11 39.1 [07 16 18 Lynds 2
 
−
L1426 . . . . . . . . . . . . . . . . 04 43 17.5 52 59 03 Lynds 1 L323 . . . . . . . . . . . . . . . . . 18 12 39.1 [18 11 47 Lynds 1
 
−
L1517 . . . . . . . . . . . . . . . . 04 52 07.2 30 33 18 BM 4 L490-2 . . . . . . . . . . . . . . 18 12 30.0 [03 46 40 Lynds 2
 
−
L1512 . . . . . . . . . . . . . . . . 05 00 54.4 32 39 00 BM 1 CB 130 . . . . . . . . . . . . . . 18 13 38.0 [02 33 52 Le 3
 
−
L1544 . . . . . . . . . . . . . . . . 05 01 14.0 25 07 00 BM 3 L328 . . . . . . . . . . . . . . . . . 18 14 06.7 [18 03 54 Lynds 1
 
−
L1523 . . . . . . . . . . . . . . . . 05 03 02.7 31 37 30 Lynds 1 L429 . . . . . . . . . . . . . . . . . 18 14 49.7 [08 15 50 Lynds 4
 
−
CB 28 . . . . . . . . . . . . . . . 05 03 51.0 [04 00 00 Le 1 L483 . . . . . . . . . . . . . . . . . 18 15 00.0 [04 40 00 Lynds 2
 
−
L1552 . . . . . . . . . . . . . . . . 05 14 34.9 26 01 17 Lynds 1 L466 . . . . . . . . . . . . . . . . . 18 17 04.5 [06 07 36 Lynds 1
 
−
L1582A . . . . . . . . . . . . . . 05 28 30.0 12 28 20 BM 1 L451 . . . . . . . . . . . . . . . . . 18 19 12.3 [07 14 11 Lynds 1
 
−
B35A . . . . . . . . . . . . . . . . 05 41 45.3 09 07 40 BM 1 L539 . . . . . . . . . . . . . . . . . 18 21 24.0 [01 06 00 Lynds 2
 
−
L1622 . . . . . . . . . . . . . . . . 05 52 00.0 01 51 00 Lynds 2 L416 . . . . . . . . . . . . . . . . . 18 22 46.2 [10 41 26 Lynds 1
 
−
L1621 . . . . . . . . . . . . . . . . 05 53 02.0 02 10 27 Lynds 2 L406 . . . . . . . . . . . . . . . . . 18 22 50.5 [11 49 11 Lynds 1
 
−
CB 37 . . . . . . . . . . . . . . . 05 57 24.0 31 39 26 Le 1 L423 . . . . . . . . . . . . . . . . . 18 25 03.9 [10 16 08 Lynds 1
 
−
L1574 . . . . . . . . . . . . . . . . 06 04 48.0 18 30 00 Lynds 1 L411 . . . . . . . . . . . . . . . . . 18 25 07.9 [11 29 15 Lynds 1
 
−
L1645 . . . . . . . . . . . . . . . . 06 05 16.0 [05 33 00 Lynds 1 L503 . . . . . . . . . . . . . . . . . 18 26 49.5 [04 40 45 Lynds 1
 
−
L1578 . . . . . . . . . . . . . . . . 06 05 33.0 18 07 00 BM 2 L443 . . . . . . . . . . . . . . . . . 18 30 00.0 [09 10 00 Lynds 2
 
−
CB 45 . . . . . . . . . . . . . . . 06 06 00.0 17 50 52 Le 1 L239 . . . . . . . . . . . . . . . . . 18 30 11.5 [26 04 16 Lynds 1
 
−
L1633 . . . . . . . . . . . . . . . . 06 22 00.0 03 30 00 Lynds 1 L588 . . . . . . . . . . . . . . . . . 18 33 00.0 [00 35 00 Lynds 1
 
−
DC 2592[132 . . . . . . 07 29 30.0 [46 51 00 HMSTG 2 L495 . . . . . . . . . . . . . . . . . 18 36 32.6 [06 41 06 Lynds 1
 
−
DC 2555[48 . . . . . . . 08 03 46.1 [39 00 10 HMSTG 1 L648 . . . . . . . . . . . . . . . . . 18 37 15.0 12 41 50 Lynds 2
 
−
V13-14. . . . . . . . . . . . . . . 08 07 39.0 [35 55 54 VMP 4 L530D . . . . . . . . . . . . . . 18 47 18.0 [04 53 20 BM 3
 
−
DC 2573[25 . . . . . . . 08 15 23.0 [39 43 36 HMSTG 2 L549 . . . . . . . . . . . . . . . . . 18 59 29.8 [05 23 08 Lynds 1
 
−
DC 2660[75 . . . . . . . 08 19 53.7 [49 41 10 HMSTG 2 L567 . . . . . . . . . . . . . . . . . 19 01 32.0 [04 30 00 BM 1
 
−
DC 2674[75 . . . . . . . 08 24 17.0 [50 52 12 HMSTG 2 B133 . . . . . . . . . . . . . . . . . 19 03 25.3 [06 57 20 BM 1
 
−
DC 2672[72 . . . . . . . 08 25 03.5 [50 30 11 HMSTG 1 CB 180 (L531) . . . . . . 19 03 31.0 [06 58 07 Le 1
 
−
DC 2676[60 . . . . . . . 08 32 38.0 [50 08 00 HMSTG 2 L581 . . . . . . . . . . . . . . . . . 19 04 55.5 [03 59 32 Lynds 1
 
−
DC 2694]30 . . . . . . . 09 20 28.7 [45 35 05 HMSTG 1 L709 . . . . . . . . . . . . . . . . . 19 11 37.3 16 22 01 Lynds 1
 
−
DC 2695]40 . . . . . . . 09 24 18.1 [44 58 32 HMSTG 1 DC 13[205 . . . . . . . . 19 13 12.4 [36 42 20 HMSTG 1
 
−
DC 2742[04 . . . . . . . 09 27 05.5 [51 23 14 HMSTG 1 L763 . . . . . . . . . . . . . . . . . 19 16 45.9 23 21 45 Lynds 1
 
−
DC 2962[158 . . . . . . 10 49 28.9 [76 48 59 HMSTG 1 L730 . . . . . . . . . . . . . . . . . 19 17 40.5 19 51 09 Lynds 2
 
−
DC 2965[157 . . . . . . 10 55 31.7 [76 48 52 HMSTG 1 L655 . . . . . . . . . . . . . . . . . 19 17 47.2 08 23 33 Lynds 1
 
−
DC 29103[35 . . . . . . 10 57 12.9 [63 26 49 HMSTG 1 L673-1-10 . . . . . . . . . . . 19 18 45.0 11 22 00 Lynds 10
 
−
TABLE 1ÈContinued
 
−
Regiona R.A. (1950) Decl. (1950) Referenceb Nc Regiona R.A. (1950) Decl. (1950) Referenceb Nc
 
−
DC 2971[161 . . . . . . 11 01 04.0 [77 25 48 HMSTG 2 L673-11 . . . . . . . 19 18 45.0 11 05 00 Lynds 1
 
−
DC 2972[151 . . . . . . 11 09 09.7 [76 37 16 HMSTG 1 L673-12 . . . . . . . 19 18 45.0 10 50 00 Lynds 3
 
−
DC 2983[131 . . . . . . 11 37 59.1 [75 00 00 HMSTG 1 L771 . . . . . . . . . . . 19 18 46.3 23 25 13 Lynds 1
 
−
DC 2977[28 . . . . . . . 11 59 07.2 [64 52 15 HMSTG 1 L684 . . . . . . . . . . . 19 19 16.1 12 23 25 Lynds 1
 
−
Mu 4 . . . . . . . . . . . . . . . . 12 21 29.0 [71 35 56 VMP 1 L677 . . . . . . . . . . . 19 19 40.0 11 25 00 Lynds 4
 
−
DC 3002[35 . . . . . . . 12 21 30.2 [65 55 26 HMSTG 1 L774 . . . . . . . . . . . 19 21 15.0 23 20 00 Lynds 2
 
−
Mu 8 . . . . . . . . . . . . . . . . 12 26 39.0 [70 54 04 VMP 2 L769 . . . . . . . . . . . 19 22 15.0 23 00 00 Lynds 4
 
−
DC 3007[10 . . . . . . . 12 28 50.6 [63 28 02 HMSTG 1 L698 . . . . . . . . . . . 19 23 37.5 12 59 48 Lynds 1
 
−
DC 3023[177 . . . . . . 12 32 17.0 [80 16 18 HMSTG 3 L778 . . . . . . . . . . . 19 25 16.0 23 40 19 Lynds 4
 
−
DC 3025[175 . . . . . . 12 37 03.2 [80 03 39 HMSTG 1 B335 . . . . . . . . . . . 19 34 33.3 07 27 00 BM 1
 
−
DC 3026[159 . . . . . . 12 41 21.4 [78 31 56 HMSTG 1 L694 . . . . . . . . . . . 19 38 18.0 10 54 44 Lynds 3
 
−
DC 3029[141 . . . . . . 12 46 14.9 [76 40 50 HMSTG 1 L758 . . . . . . . . . . . 19 44 12.8 18 54 47 Lynds 1
 
−
Ch 5 . . . . . . . . . . . . . . . . . 12 46 38.7 [76 41 04 VMP 1 L880 . . . . . . . . . . . 20 11 49.4 40 03 59 Lynds 1
 
−
DC 3030[143 . . . . . . 12 49 14.6 [76 56 33 HMSTG 1 L1152 . . . . . . . . . 20 35 24.0 67 43 53 BM 1
 
−
Ch 17 . . . . . . . . . . . . . . . . 12 56 14.0 [77 00 00 VMP 4 L1041 . . . . . . . . . 20 36 05.5 57 33 36 Lynds 1
 
−
DC 3036[145 . . . . . . 12 59 11.0 [77 06 44 HMSTG 2 L922 . . . . . . . . . . . 20 36 22.0 44 19 07 Lynds 1
 
−
DC 3037[148 . . . . . . 13 01 39.7 [77 26 49 HMSTG 2 L917 . . . . . . . . . . . 20 38 30.0 43 58 00 Lynds 2
 
−
DC 3037[150 . . . . . . 13 01 55.0 [77 36 42 HMSTG 2 L1049 . . . . . . . . . 20 40 00.0 57 20 00 Lynds 2
 
−
DC 3038[142 . . . . . . 13 03 36.4 [76 44 48 HMSTG 1 L1148 . . . . . . . . . 20 40 00.0 67 11 00 BM 2
 
−
DC 3162]51 . . . . . . . 14 22 33.6 [55 07 04 HMSTG 1 L896 . . . . . . . . . . . 20 40 28.8 39 42 22 Lynds 2
 
−
DC 3148[51 . . . . . . . 14 44 23.4 [65 04 41 HMSTG 1 L1155C . . . . . . . 20 43 00.0 67 41 44 BM 3
 
−
DC 3230]40 . . . . . . . 15 07 35.6 [53 06 36 HMSTG 1 L915 . . . . . . . . . . . 20 43 23.0 42 58 52 Lynds 1
 
−
DC 3382]164 . . . . . . 15 37 21.0 [34 29 18 HMSTG 2 L1082C . . . . . . . 20 49 36.0 60 07 40 BM 3
 
−
DC 3272]18 . . . . . . . 15 38 33.4 [52 38 36 HMSTG 1 L1082AB . . . . . . 20 52 20.7 60 03 14 BM 2
 
−
DC 3388]165 . . . . . . 15 39 25.0 [33 52 00 HMSTG 6 L981 . . . . . . . . . . . 20 58 38.0 50 05 09 Lynds 3
 
−
DC 3392]161 . . . . . . 15 42 01.0 [34 08 00 HMSTG 4 L971 . . . . . . . . . . . 20 59 15.8 49 07 34 Lynds 2
 
−
DC 3389]151 . . . . . . 15 43 49.0 [35 04 30 HMSTG 2 L1174 . . . . . . . . . 20 59 46.3 68 01 04 BM 1
 
−
L134A . . . . . . . . . . . . . . . 15 50 58.1 [04 26 36 BM 1 L1172A . . . . . . . 21 01 45.0 67 35 13 BM 3
 
−
L183 . . . . . . . . . . . . . . . . . 15 51 35.7 [02 40 54 BM 1 L1063 . . . . . . . . . 21 06 44.6 56 06 09 Lynds 1
 
−
DC 3386]119 . . . . . . 15 53 26.0 [37 41 12 HMSTG 2 B361 . . . . . . . . . . . 21 10 35.0 47 12 01 BM 2
 
−
DC 3356]82 . . . . . . . 15 54 42.3 [42 26 57 HMSTG 1 L1125 . . . . . . . . . 21 14 07.0 61 27 10 Lynds 2
 
−
DC 3391]117 . . . . . . 15 55 22.0 [37 31 12 HMSTG 2 L944 . . . . . . . . . . . 21 15 54.0 43 05 41 Lynds 3
 
−
DC 3364]82 . . . . . . . 15 58 00.0 [41 50 00 HMSTG 2 L952-3 . . . . . . . . 21 18 51.0 43 13 00 Lynds 3
 
−
DC 3369]83 . . . . . . . 15 59 05.3 [41 31 30 HMSTG 1 L1021 . . . . . . . . . 21 20 34.8 50 50 17 Lynds 1
 
−
DC 3386]95 . . . . . . . 16 01 09.6 [39 29 37 HMSTG 1 L1014-1 . . . . . . . 21 22 20.6 49 56 52 Lynds 2
 
−
DC 3346]46 . . . . . . . 16 02 54.2 [45 46 25 HMSTG 1 L1099 . . . . . . . . . 21 34 27.9 57 13 18 Lynds 2
 
−
DC 3394]95 . . . . . . . 16 04 27.0 [39 04 06 HMSTG 1 L973 . . . . . . . . . . . 21 35 16.3 43 06 57 Lynds 1
 
−
DC 3376]76 . . . . . . . 16 04 58.6 [41 32 54 HMSTG 1 L1111 . . . . . . . . . 21 38 53.6 57 34 24 Lynds 1
 
−
DC 3397]92 . . . . . . . 16 06 45.0 [38 58 24 HMSTG 3 L1121 . . . . . . . . . 21 39 10.0 58 02 33 Lynds 1
 
−
DC 3381]71 . . . . . . . 16 07 59.4 [41 34 19 HMSTG 3 L1103 . . . . . . . . . 21 40 40.6 56 30 00 Lynds 2
 
−
DC 3402]90 . . . . . . . 16 08 01.0 [38 53 49 HMSTG 1 L1113 . . . . . . . . . 21 42 56.7 56 56 25 Lynds 2
 
−
DC 3369]51 . . . . . . . 16 10 18.3 [43 53 34 HMSTG 1 L1031C . . . . . . . 21 44 35.6 47 04 20 BM 1
 
−
DC 3420]94 . . . . . . . 16 14 28.7 [37 23 52 HMSTG 1 L1139 . . . . . . . . . 21 53 47.3 58 20 14 Lynds 2
 
−
DC 3412]65 . . . . . . . 16 21 44.4 [39 52 38 HMSTG 1 L1143 . . . . . . . . . 21 57 03.0 58 42 25 Lynds 1
 
−
L1681A* . . . . . . . . . . . . 16 23 59.0 [24 27 32 BM 1 L1166 . . . . . . . . . 22 03 46.7 59 19 07 Lynds 1
 
−
L1681B . . . . . . . . . . . . . . 16 24 33.8 [24 36 47 BM 1 L1164 . . . . . . . . . 22 05 07.7 58 51 15 Lynds 1
 
−
L1696AB . . . . . . . . . . . . 16 25 30.0 [24 12 32 BM 3 L1235 . . . . . . . . . 22 14 41.4 73 10 00 BM 1
 
−
L1704 . . . . . . . . . . . . . . . . 16 27 50.0 [23 34 37 BM 2 L1195 . . . . . . . . . 22 25 18.1 61 01 06 Lynds 1
 
−
L1757 . . . . . . . . . . . . . . . . 16 29 01.9 [19 35 24 Lynds 2 L1221 . . . . . . . . . 22 26 38.4 68 45 48 Lynds 1
 
−
L1709BC* . . . . . . . . . . 16 29 16.0 [23 51 12 BM 4 L1185 . . . . . . . . . 22 27 27.6 58 53 30 Lynds 1
 
−
L1689AB* . . . . . . . . . . 16 30 10.5 [24 37 57 BM 6 L1251A . . . . . . . 22 29 03.3 74 58 51 BM 2
 
−
DC 3387]18 . . . . . . . 16 30 33.3 [44 54 53 HMSTG 1 L1197 . . . . . . . . . 22 35 08.0 58 41 46 Lynds 1
 
−
L43 . . . . . . . . . . . . . . . . . . 16 31 27.7 [15 41 40 BM 3 L1251 . . . . . . . . . 22 36 26.0 74 54 46 Lynds 1
 
−
DC 3460]78 . . . . . . . 16 33 32.0 [35 31 06 HMSTG 2 L1229 . . . . . . . . . 23 12 16.8 61 46 47 Lynds 1
 
−
DC 3464]79 . . . . . . . 16 34 13.4 [35 08 26 HMSTG 1 L1234 . . . . . . . . . 23 15 12.0 62 10 00 Lynds 1
 
−
DC 3463]78 . . . . . . . 16 34 26.8 [35 21 54 HMSTG 1 CB 243 . . . . . . . . 23 23 00.0 63 20 00 Le 1
 
−
L121 . . . . . . . . . . . . . . . . . 16 36 41.0 [13 59 21 Lynds 1 L1262A . . . . . . . 23 23 32.2 74 01 45 BM 1
 
−
L1782 . . . . . . . . . . . . . . . . 16 39 13.2 [19 36 22 Lynds 2 CB 246 . . . . . . . . 23 54 12.0 58 17 47 Le 1
 
−
DC 3393[03 . . . . . . . 16 42 30.0 [45 54 54 HMSTG 1 L1263 . . . . . . . . . 23 54 54.2 64 32 27 Lynds 1
 
−
DC 3405]05 . . . . . . . 16 43 05.8 [44 26 04 HMSTG 1 L1271 . . . . . . . . . 23 59 15.3 67 01 48 Lynds 4
 
−
NOTE.ÈUnits of right ascension are hours, minutes, and seconds, and units of declination are degrees, arcminutes, and arcseconds.
 
−
a Searched size of all regions is 30@]30@ except for the Ðve regions marked with an asterisk behind the name of the region, whose searched area is
 
−
60@]60@.
 
−
b REFERENCES.ÈLynds, Lynds 1962; BM, Benson & Myers 1989; Le, Lemme et al. 1996; ON, Onishi et al. 1996; CO, Codella et al. 1997; HMSTG,
 
−
Hartley et al. 1986; VMP, Vilas-Boas et al. 1994.
 
−
c Number of cores selected in each reference region.
 
−
L1622
 
−
A
 
−
B
 
−
OPTICALLY SELECTED CORES 237
 
−
FIG. 1.ÈAn example (for L1622) of how to select the local minimum positions of the intensity in a cloud by its optical extinction using an image extracted
 
−
from the STScI Digitized Sky Survey. The area of the image is and the coordinate of 0¡.5]0¡.5 the center is (a, d) 52m 01¡ 51@ 00@@), which was 1950.0\(5h 00s.0,
 
−
changed from the Lynds (1962) position to shift the cloud into a central position in the image. The smooth contours are overlaid on the gray-scale image to
 
−
enable identiÐcation of two local minima (A and B) of intensity. The smoothing length for the contours in this case is 30A. The regions with the locally lowest
 
−
or highest intensity are marked with L and H, respectively. The numeric values below the characters are data values by DSS that are proportional to
 
−
photographic densities.
 
−
2.2.1. T he Darkness Contrast of Cores
 
−
In Table 2, column (10), we give an indication of a darkness
 
−
contrast (DC) of the dark core to the background in
 
−
the DSS image. This contrast was calculated according to
 
−
(IB[IC)/IB, where IB and IC are the data values (DN) by
 
−
DSS (that are on a scale of photographic density [c] in the
 
−
expression c\DN/6553.4 [Postman 1996]) for the background
 
−
and the core, respectively. The IB and IC values were
 
−
approximately determined by using a cut-proÐle of the data
 
−
values crossing the core. The IB and IC would correspond to
 
−
a constantly Ñat level and a minimum level of the proÐle,
 
−
respectively. Figure 2 shows an example of how we adopted
 
−
IB and IC for L1622. This cut-proÐle is the one crossing two
 
−
intensity minima of L1622A and L1622B.
 
−
According to this value of the DC, we classiÐed cores into
 
−
four quartiles, 1 being the least dark to 4 the most dark so
 
−
that each group contains 25% of total number of cores. It is
 
−
noted that the Lynds 6 and HMSTG A clouds more likely
 
−
consist of cores with a DC of 3 or 4, while Lynds 5 clouds
 
−
more likely have cores with a DC of 1 or 2 (Fig. 3). However
 
−
we also note that if the dark cores are located at the dark
 
−
background, the DC values tend to have a low value. This
 
−
explains why many Lynds 6 cores also have a DC value of 1
 
−
in Figure 3.
 
−
2.2.2. T he Size and the AspectRatio of Cores
 
−
For evaluation of these properties, we do not consider
 
−
cores with more than two peaks in the contour map because
 
−
of ambiguity in the size information of such cores, but we do
 
−
consider cores with only one peak in the map whose size
 
−
and aspect ratio can be better determined. The distribution
 
−
of the apparent angular size of cores is shown with the
 
−
geometric mean (ab)0.5 of cores in Figure 4, indicating that
 
−
most of the cores (D70%) have angular size between 1@ and
 
−
TABLE 2
 
−
OPTICALLY SELECTED CORES
 
−
a b R PA Distance
 
−
Number Source R.A. (1950) Decl. (1950) (arcmin) (arcmin) (arcmin) (deg) EYSO DC Class (pc) References
 
−
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
 
−
1 . . . . . . . . L1275 00 00 48.2 67 02 05 8.2 1.5 3.5 25 N 4 5 . . . . . .
 
−
2 . . . . . . . . L1291 00 39 47.6 61 44 35 1.5 1.5 1.5 0 N 2 5 . . . . . .
 
−
3 . . . . . . . . L1333 02 21 10.2 75 13 32 2.8 1.7 2.2 2 N 3 6 . . . . . .
 
−
4 . . . . . . . . L1355 02 48 41.4 68 43 36 3.5 1.6 2.4 8 N 3 6 300 1
 
−
5 . . . . . . . . L1358-1 02 51 13.3 69 01 38 1.9 1.4 1.6 14 Y 2 6 . . . . . .
 
−
6 . . . . . . . . L1358-2 02 51 55.1 69 12 03 2.8 1.3 1.9 [87 N 2 6 . . . . . .
 
−
7 . . . . . . . . B5-1 03 44 26.4 32 46 45 3.2 1.6 2.3 [43 N 1 . . . 350 2
 
−
8 . . . . . . . . B5-2 03 45 15.5 32 45 07 2.1 1.8 1.9 24 N 1 . . . 350 2
 
−
9 . . . . . . . . CB 17 (L1389) 04 00 35.4 56 47 50 1.7 0.6 1.0 [44 Y 3 6 170 3
 
−
10 . . . . . . L1498 04 07 51.8 25 01 35 3.2 1.6 2.3 [71 N 1 5 140 4
 
−
11 . . . . . . L1495-2 04 14 51.2 28 30 40 6.3 5.1 5.7 7 N 3 5 140 4
 
−
12 . . . . . . L1495-3 04 15 23.9 28 21 21 12.0 5.7 8.3 15 Y 3 5 140 4
 
−
13 . . . . . . L1506B 04 16 03.9 25 13 01 7.9 2.2 4.2 [85 N 1 6 140 4
 
−
14 . . . . . . L1399-1 04 20 00.5 55 01 00 . . . . . . 6.2 . . . N 1 5 170 3
 
−
15 . . . . . . L1506A 04 20 30.1 24 58 29 20.2 9.5 13.9 [64 Y 2 6 140 4
 
−
16 . . . . . . L1521B-2 04 20 32.8 26 33 11 . . . . . . 6.2 . . . N 2 4 140 4
 
−
17 . . . . . . L1399-2 04 20 58.3 54 52 48 . . . . . . 9.2 . . . N 2 5 170 3
 
−
18 . . . . . . L1521B-1 04 21 11.6 26 29 12 4.7 4.7 4.7 0 N 2 4 140 4
 
−
19 . . . . . . L1399-3 04 21 11.8 54 49 59 . . . . . . 9.2 . . . N 2 5 170 3
 
−
20 . . . . . . B213-7 04 22 12.8 26 26 10 . . . . . . 5.4 . . . N 1 . . . 140 4
 
−
21 . . . . . . B217-1 04 24 44.5 26 11 27 3.2 1.7 2.3 [21 Y 1 . . . 140 4
 
−
22 . . . . . . B217-2 04 25 04.5 26 14 16 3.3 1.9 2.5 38 N 2 . . . 140 4
 
−
23 . . . . . . L1400A-2 04 25 05.8 54 39 40 4.1 1.3 2.3 [81 N 3 3 170 3
 
−
24 . . . . . . L1521-1 (L1521F) 04 25 29.0 26 45 04 6.9 4.4 5.5 [55 N 1 4 140 4
 
−
25 . . . . . . L1400F (L1407) 04 25 37.0 54 07 23 15.2 10.1 12.4 65 N 2 3 170 3
 
−
26 . . . . . . L1524-2 04 26 16.9 24 25 02 6.3 5.2 5.7 [86 Y 2 5 140 4
 
−
27 . . . . . . L1521E 04 26 17.2 26 07 34 2.7 1.7 2.1 90 N 1 4 140 4
 
−
28 . . . . . . L1524-1 04 26 17.8 24 31 26 6.5 3.6 4.8 [71 Y 2 5 140 4
 
−
29 . . . . . . L1521-2 04 26 26.8 26 53 27 5.5 2.5 3.7 [69 N 1 4 140 4
 
−
30 . . . . . . L1400K 04 26 41.6 54 44 16 . . . . . . 5.2 . . . N 4 3 170 3
 
−
31 . . . . . . L1524-3 04 26 51.5 24 23 44 10.8 5.4 7.6 [36 Y 2 5 140 4
 
−
32 . . . . . . L1524-4 04 27 04.1 24 18 47 10.8 5.4 7.6 [36 N 2 5 140 4
 
−
33 . . . . . . L1551S-2 04 28 03.5 18 09 09 5.7 3.8 4.7 [11 N 1 6 140 4
 
−
34 . . . . . . L1445 04 28 28.8 46 31 01 8.2 2.2 4.2 [10 N 2 5 . . . . . .
 
−
35 . . . . . . TMC 2-2 (L1529) 04 28 35.8 24 17 29 4.6 2.1 3.1 63 Y 1 5 140 4
 
−
36 . . . . . . L1551S-1 04 28 53.9 18 01 14 2.8 1.3 1.9 [41 N 1 6 140 4
 
−
37 . . . . . . TMC 2A (L1529) 04 28 59.1 24 25 42 9.5 4.7 6.7 [40 Y 1 5 140 4
 
−
38 . . . . . . B18-2 04 29 34.4 24 45 46 3.8 1.7 2.5 [55 N 2 . . . 140 4
 
−
39 . . . . . . TMC 2-1 (L1529) 04 29 37.5 24 18 14 . . . . . . 7.0 . . . Y 1 5 140 4
 
−
40 . . . . . . L1536-2 04 29 50.7 22 53 29 2.7 2.0 2.3 [2 N 1 4 140 4
 
−
41 . . . . . . TMC 2-3 (L1529) 04 29 57.6 24 11 26 4.3 2.5 3.3 [70 N 1 5 140 4
 
−
42 . . . . . . L1536-3 04 30 01.7 22 47 41 2.4 0.9 1.5 76 N 1 4 140 4
 
−
43 . . . . . . L1536-1 04 30 19.7 22 36 51 11.4 5.1 7.6 [88 N 1 4 140 4
 
−
44 . . . . . . B18-3 04 31 04.6 24 03 32 7.9 1.9 3.9 [55 N 3 . . . 140 4
 
−
45 . . . . . . B18-4 04 32 34.0 24 02 48 4.1 3.8 3.9 2 Y 3 . . . 140 4
 
−
46 . . . . . . B18-5 04 32 49.7 24 03 15 3.0 2.1 2.5 [37 N 2 . . . 140 4
 
−
47 . . . . . . L1527A-1 04 35 05.1 26 08 37 7.6 4.4 5.8 [75 Y 1 6 140 4
 
−
48 . . . . . . L1527A-2 04 35 54.0 26 15 38 4.0 1.5 2.4 5 N 1 6 140 4
 
−
49 . . . . . . L1534 04 36 36.4 25 35 14 9.5 6.3 7.7 [73 Y 1 5 140 4
 
−
50 . . . . . . CB 22 (L1503) 04 37 30.2 29 47 13 4.7 1.7 2.8 [43 N 2 5 140 4
 
−
51 . . . . . . TMC 1-1 (L1527) 04 38 26.5 25 39 27 15.8 4.7 8.6 [40 Y 2 6 140 4
 
−
52 . . . . . . TMC 1C (L1527) 04 38 27.5 25 55 46 12.6 5.7 8.5 [52 Y 2 6 140 4
 
−
53 . . . . . . L1507-1 04 39 29.4 29 36 24 4.7 2.2 3.2 [13 N 2 5 140 4
 
−
54 . . . . . . L1507-2 04 39 53.4 29 38 25 3.5 1.6 2.4 71 N 1 5 140 4
 
−
55 . . . . . . L1507-3 04 40 21.4 29 33 37 1.7 0.9 1.2 38 N 2 5 140 4
 
−
56 . . . . . . L1426 04 43 17.5 52 59 03 2.1 2.1 2.1 0 N 1 5 170 3
 
−
57 . . . . . . L1517C 04 51 33.6 30 30 54 4.7 3.2 3.9 [69 N 2 6 140 4
 
−
58 . . . . . . L1517B-2 04 51 56.4 30 38 03 3.2 2.1 2.6 [45 N 1 6 140 4
 
−
59 . . . . . . L1517A 04 51 56.7 30 29 20 4.7 2.5 3.4 [64 N 2 6 140 4
 
−
60 . . . . . . L1517B-1 04 52 05.9 30 32 58 4.7 1.7 2.8 [4 N 3 6 140 4
 
−
61 . . . . . . L1517D 04 52 45.7 30 35 14 4.7 2.4 3.4 [45 N 2 6 140 4
 
−
62 . . . . . . L1544-3 05 00 38.6 25 14 18 4.7 2.4 3.4 90 N 1 6 140 4
 
−
63 . . . . . . L1512 (CB 27) 05 00 54.4 32 39 00 4.7 2.2 3.2 [13 N 3 6 140 4
 
−
64 . . . . . . L1544-1 05 01 18.3 25 07 29 . . . . . . 5.8 . . . N 1 6 140 4
 
−
65 . . . . . . L1544-2 05 01 39.1 25 07 30 2.4 1.9 2.1 [60 N 1 6 140 4
 
−
238
 
−
TABLE 2ÈContinued
 
−
a b R PA Distance
 
−
Number Source R.A. (1950) Decl. (1950) (arcmin) (arcmin) (arcmin) (deg) EYSO DC Class (pc) References
 
−
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
 
−
66 . . . . . . . L1523 05 03 02.7 31 37 30 5.1 1.9 3.1 12 N 2 6 140 4
 
−
67 . . . . . . . CB 28 05 03 51.2 [04 00 20 3.6 2.4 2.9 83 N 2 . . . 500 5
 
−
68 . . . . . . . L1552 05 14 34.9 26 01 17 5.9 2.5 3.8 [1 N 3 6 140 4
 
−
69 . . . . . . . L1582A 05 29 15.0 12 28 57 5.2 2.4 3.5 [52 N 4 5 400 6
 
−
70 . . . . . . . B35A 05 41 50.5 09 09 17 3.2 1.6 2.3 11 Y 2 . . . 400 7
 
−
71 . . . . . . . L1622A 05 52 17.1 01 56 55 5.1 1.1 2.4 39 N 3 6 500 5
 
−
72 . . . . . . . L1622B 05 52 17.5 01 45 11 2.2 1.1 1.6 87 Y 3 6 500 5
 
−
73 . . . . . . . L1621-2 05 52 49.8 02 08 07 1.0 0.8 0.9 90 N 2 4 500 5
 
−
74 . . . . . . . L1621-1 05 53 23.0 02 17 39 5.9 1.1 2.5 25 N 3 4 500 5
 
−
75 . . . . . . . CB 37 (L1555) 05 57 29.9 31 39 25 4.7 3.1 3.8 [87 N 3 4 . . . . . .
 
−
76 . . . . . . . L1574 06 05 08.9 18 28 41 2.5 0.9 1.5 [11 N 1 4 . . . . . .
 
−
77 . . . . . . . L1645 06 05 16.2 [05 32 16 4.9 1.3 2.5 6 Y 1 4 830 9
 
−
78 . . . . . . . L1578-2 06 05 40.4 18 12 00 13.3 5.7 8.7 7 PM* 3 4 . . . . . .
 
−
79 . . . . . . . L1578-1 06 05 41.6 18 06 54 13.3 5.7 8.7 7 PM* 2 4 . . . . . .
 
−
80 . . . . . . . CB 45 (L1578) 06 06 02.0 17 50 48 2.4 1.6 2.0 [38 N 3 4 . . . . . .
 
−
81 . . . . . . . L1633 06 22 04.0 03 23 53 1.4 1.4 1.4 0 N 3 4 . . . . . .
 
−
82 . . . . . . . DC 2592[132-1 (V4) 07 29 02.8 [46 37 10 1.6 0.5 0.9 88 N 4 A 300 10
 
−
83 . . . . . . . DC 2592[132-2 (V4) 07 29 20.3 [46 49 26 2.2 1.6 1.9 [31 N 3 A 300 10
 
−
84 . . . . . . . DC 2555[48 08 03 46.1 [39 00 10 5.2 0.9 2.2 86 N 3 A 300 10
 
−
85 . . . . . . . V13-2 08 06 54.9 [35 54 21 2.5 1.4 1.9 [54 N 4 A 300 10
 
−
86 . . . . . . . V13-3 08 07 01.0 [35 48 22 3.2 0.7 1.5 [28 N 4 A 300 10
 
−
87 . . . . . . . V13-1 08 07 09.0 [35 52 18 0.8 0.6 0.7 7 N 4 A 300 10
 
−
88 . . . . . . . V14 08 07 39.9 [35 56 04 . . . . . . 1.8 . . . Y 4 A 300 10
 
−
89 . . . . . . . DC 2573[25-1 08 15 19.5 [39 44 40 2.5 1.6 2.0 43 Y 4 A 300 10
 
−
90 . . . . . . . DC 2573[25-2 08 15 23.8 [39 41 40 1.3 0.9 1.1 39 N 3 A 300 10
 
−
91 . . . . . . . DC 2660[75-2 08 19 40.0 [49 31 38 . . . . . . 5.0 . . . Y 3 A 300 10
 
−
92 . . . . . . . DC 2660[75-1 08 19 53.7 [49 41 10 . . . . . . 7.0 . . . N 3 A 300 10
 
−
93 . . . . . . . DC 2674[75 08 24 15.2 [50 52 08 5.6 2.4 3.7 32 Y 4 A 300 10
 
−
94 . . . . . . . DC 2672[72 08 25 03.5 [50 30 11 . . . . . . 2.0 . . . Y 4 A 300 10
 
−
95 . . . . . . . DC 2675[74 08 25 10.2 [50 52 00 1.9 1.1 1.4 4 N 4 A 300 10
 
−
96 . . . . . . . DC 2676[60-1 08 32 36.6 [50 08 03 1.9 1.1 1.4 [73 N 4 A 300 10
 
−
97 . . . . . . . DC 2676[60-2 08 32 45.3 [50 14 33 1.4 0.8 1.1 32 N 4 A 300 10
 
−
98 . . . . . . . DC 2694]30 (V27) 09 20 28.7 [45 35 05 8.1 1.6 3.6 [34 N 4 A 300 10
 
−
99 . . . . . . . DC 2695]40 09 24 18.1 [44 58 32 6.3 0.9 2.4 72 N 3 A 300 10
 
−
100 . . . . . . DC 2742[04 09 27 05.5 [51 23 14 4.6 1.9 3.0 12 N 4 A 300 10
 
−
101 . . . . . . DC 2962[158 10 49 28.9 [76 48 59 . . . . . . 4.6 . . . N 3 A 150 11
 
−
102 . . . . . . DC 2965[157 10 55 31.7 [76 48 52 4.7 1.9 3.0 [2 N 2 A 150 11
 
−
103 . . . . . . DC 29103[35 10 57 12.9 [63 26 49 10.7 2.5 5.2 [76 N 1 A . . . . . .
 
−
104 . . . . . . DC 2971[161-1 11 01 09.3 [77 26 22 9.5 3.2 5.5 34 N 3 A 150 11
 
−
105 . . . . . . DC 2971[161-2 11 01 39.8 [77 32 55 . . . . . . 5.8 . . . N 3 A 150 11
 
−
106 . . . . . . DC 2972[151 11 09 47.9 [76 38 29 10.1 4.7 6.9 [48 N 2 A 150 11
 
−
107 . . . . . . DC 2983[131 11 37 59.1 [75 00 00 3.5 2.7 3.1 [56 N 3 A 150 11
 
−
108 . . . . . . DC 2977[28 11 59 07.2 [64 52 15 6.9 3.2 4.7 [47 Y 1 A 175 12
 
−
109 . . . . . . Mu 4 12 21 29.0 [71 35 56 3.9 0.8 1.8 25 N 1 A 225 13
 
−
110 . . . . . . DC 3002[35 12 21 30.2 [65 55 26 7.3 1.3 3.1 [78 N 1 A 175 12
 
−
111 . . . . . . Mu 8 12 26 39.0 [70 54 04 8.4 1.0 2.9 39 N 1 A 225 13
 
−
112 . . . . . . Mu 10 12 28 03.4 [70 46 30 . . . . . . 8.4 . . . N 1 A 225 13
 
−
113 . . . . . . DC 3020[177-1 12 28 22.6 [80 19 54 2.8 1.3 1.9 [40 N 3 A 200 14
 
−
114 . . . . . . DC 3007[10 (Co2) 12 28 50.6 [63 28 02 10.1 6.6 8.2 [32 N 1 A 175 12
 
−
115 . . . . . . DC 3023[177 12 31 54.0 [80 13 31 3.3 1.6 2.3 26 N 3 A 200 14
 
−
116 . . . . . . DC 3020[177-2 12 33 06.8 [80 20 35 1.9 1.3 1.6 48 N 3 A 200 14
 
−
117 . . . . . . DC 3025[175 12 37 03.2 [80 03 39 3.0 0.6 1.3 52 N 3 A 200 14
 
−
118 . . . . . . DC 3026[159 12 41 21.4 [78 31 56 2.1 1.3 1.7 [51 N 3 A 200 14
 
−
119 . . . . . . Ch 5 12 46 38.7 [76 41 04 9.3 3.5 5.7 65 N 2 A 200 14
 
−
120 . . . . . . DC 3030[143 (Ch 7) 12 49 14.6 [76 56 33 8.5 6.0 7.1 [59 Y 1 A 200 14
 
−
121 . . . . . . Ch 17 12 54 44.8 [76 56 34 5.7 3.2 4.3 [32 N 2 A 200 14
 
−
122 . . . . . . Ch 19-2 12 56 59.5 [77 02 36 9.5 3.8 6.0 [24 N 2 A 200 14
 
−
123 . . . . . . Ch 19-1 12 57 24.1 [76 57 01 9.5 3.8 6.0 [24 Y 2 A 200 14
 
−
124 . . . . . . Ch 20 12 59 18.9 [77 06 56 2.8 1.7 2.2 [32 N 2 A 200 14
 
−
125 . . . . . . DC 3037[145 13 01 12.6 [77 09 35 4.6 2.8 3.6 17 N 2 A 200 14
 
−
126 . . . . . . DC 3037[148 13 01 39.7 [77 26 49 3.2 1.6 2.3 [22 N 1 A 200 14
 
−
127 . . . . . . DC 3037[152 13 01 51.6 [77 45 01 . . . . . . 5.0 . . . N 2 A 200 14
 
−
128 . . . . . . DC 3037[150 13 02 00.5 [77 37 08 4.7 3.7 4.2 0 N 2 A 200 14
 
−
129 . . . . . . DC 3038[142 13 03 36.4 [76 44 48 4.7 2.4 3.4 78 Y 2 A 200 14
 
−
130 . . . . . . DC 3162]51 14 22 33.6 [55 07 04 . . . . . . 4.8 . . . N 4 A . . . . . .
 
−
131 . . . . . . DC 3148[51 14 44 23.4 [65 04 41 10.1 2.2 4.7 [82 Y 1 A 170 15
 
−
239
 
−
TABLE 2ÈContinued
 
−
a b R PA Distance
 
−
Number Source R.A. (1950) Decl. (1950) (arcmin) (arcmin) (arcmin) (deg) EYSO DC Class (pc) References
 
−
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
 
−
132 . . . . . . DC 3230]40 15 07 35.6 [53 06 36 2.4 1.1 1.6 55 N 3 A . . . . . .
 
−
133 . . . . . . DC 3379]164 15 36 25.2 [34 36 48 3.8 2.8 3.3 [18 Y 3 A 170 16
 
−
134 . . . . . . DC 3382]164 15 37 23.9 [34 30 40 4.7 2.1 3.1 4 N 4 A 170 16
 
−
135 . . . . . . DC 3272]18 15 38 33.4 [52 38 36 . . . . . . 3.0 . . . N 4 A . . . . . .
 
−
136 . . . . . . DC 3388]165-2 15 39 08.8 [33 41 27 4.1 3.2 3.6 [67 N 3 A 170 16
 
−
137 . . . . . . DC 3388]165-3 15 39 29.2 [33 42 30 5.7 2.5 3.8 [50 N 3 A 170 16
 
−
138 . . . . . . DC 3388]165-4 15 39 32.4 [33 59 44 . . . . . . 8.8 . . . Y 3 A 170 16
 
−
139 . . . . . . DC 3388]165-5 15 39 49.9 [33 59 18 . . . . . . 8.8 . . . Y 3 A 170 16
 
−
140 . . . . . . DC 3388]165-6 15 40 06.5 [34 04 01 2.5 1.9 2.2 [86 N 2 A 170 16
 
−
141 . . . . . . DC 3392]161-1 15 41 42.7 [34 08 10 10.1 5.7 7.6 40 Y 3 A 170 16
 
−
142 . . . . . . DC 3392]161-2 15 42 01.1 [34 03 59 4.1 2.5 3.2 52 N 3 A 170 16
 
−
143 . . . . . . DC 3392]161-3 15 42 03.2 [34 11 21 2.4 1.4 1.8 [72 N 3 A 170 16
 
−
144 . . . . . . DC 3392]161-4 15 42 16.9 [34 15 19 6.5 3.6 4.8 19 N 3 A 170 16
 
−
145 . . . . . . DC 3389]151 15 43 24.3 [35 02 46 7.9 1.4 3.3 [47 N 3 A 170 16
 
−
146 . . . . . . DC 3390]150 15 44 46.3 [35 03 29 5.1 2.2 3.3 [7 Y 4 A 170 16
 
−
147 . . . . . . L134A 15 50 49.0 [04 25 00 4.9 4.9 4.9 0 N 1 5 165 17
 
−
148 . . . . . . L183 15 51 22.8 [02 40 44 6.3 3.8 4.9 51 N 2 5 165 17
 
−
149 . . . . . . DC 3386]119-1 15 53 25.0 [37 45 27 6.5 2.4 3.9 21 N 3 A 170 16
 
−
150 . . . . . . DC 3386]119-2 15 53 40.4 [37 39 54 5.1 3.2 4.0 64 Y 4 A 170 16
 
−
151 . . . . . . DC 3356]82 15 54 42.3 [42 26 57 7.1 1.7 3.5 [88 N 3 A 170 16
 
−
152 . . . . . . DC 3391]117-1 15 55 22.3 [37 30 42 2.5 1.6 2.0 71 N 4 A 170 16
 
−
153 . . . . . . DC 3391]117-2 15 55 45.6 [37 28 26 4.1 2.4 3.1 33 N 4 A 170 16
 
−
154 . . . . . . DC 3364]82 15 57 26.9 [41 55 44 17.7 11.1 14.0 90 N 4 A 170 16
 
−
155 . . . . . . DC 3367]82 15 58 00.8 [41 44 44 15.8 3.8 7.7 57 N 4 A 170 16
 
−
156 . . . . . . DC 3369]83 15 59 05.3 [41 31 30 6.3 2.8 4.2 [31 N 4 A 170 16
 
−
157 . . . . . . DC 3386]95 16 01 09.6 [39 29 37 . . . . . . 4.0 . . . N 4 A 170 16
 
−
158 . . . . . . DC 3346]46 16 02 54.2 [45 46 25 6.9 3.8 5.1 44 N 2 A 170 16
 
−
159 . . . . . . DC 3394]95 16 04 27.0 [39 04 06 4.3 2.4 3.2 [29 N 3 A 170 16
 
−
160 . . . . . . DC 3376]76 16 04 58.6 [41 32 54 8.2 3.8 5.6 22 N 4 A 170 16
 
−
161 . . . . . . DC 3397]92-1 16 06 19.9 [39 01 37 . . . . . . 11.8 . . . Y 3 A 170 16
 
−
162 . . . . . . DC 3397]92-2 16 06 45.1 [38 55 58 . . . . . . 11.8 . . . Y 3 A 170 16
 
−
163 . . . . . . DC 3397]92-3 16 07 01.5 [39 03 00 . . . . . . 11.8 . . . Y 3 A 170 16
 
−
164 . . . . . . DC 3381]71 16 07 59.4 [41 34 19 14.5 8.2 10.9 80 N 3 A 170 16
 
−
165 . . . . . . DC 3402]90-1 16 08 01.0 [38 53 49 . . . . . . 8.2 . . . PM 3 A 170 16
 
−
166 . . . . . . DC 3402]90-2 16 08 15.2 [38 50 38 . . . . . . 8.2 . . . PM 3 A 170 16
 
−
167 . . . . . . DC 3402]90-3 16 08 23.4 [38 53 56 . . . . . . 8.2 . . . PM 3 A 170 16
 
−
168 . . . . . . DC 3369]51 16 10 18.3 [43 53 34 11.4 3.2 6.0 [60 N 3 A 170 16
 
−
169 . . . . . . DC 3420]94 16 14 28.7 [37 23 52 4.4 3.3 3.8 [11 N 3 A 170 16
 
−
170 . . . . . . DC 3412]65 16 21 44.4 [39 52 38 11.4 3.2 6.0 [52 N 1 A 170 16
 
−
171 . . . . . . L1681A 16 23 58.5 [24 27 39 . . . . . . 26.6 . . . Y 4 5 165 17
 
−
172 . . . . . . L1696B-1 16 24 40.3 [24 06 24 . . . . . . 11.0 . . . Y 4 6 165 17
 
−
173 . . . . . . L1696A 16 25 27.5 [24 12 48 . . . . . . 11.0 . . . N 4 6 165 17
 
−
174 . . . . . . L1696B-2 16 26 09.4 [24 06 43 6.6 3.8 5.0 [35 N 4 6 165 17
 
−
175 . . . . . . L1704-1 16 27 49.8 [23 35 49 4.9 3.2 4.0 32 N 4 6 165 17
 
−
176 . . . . . . L1704-2 16 28 09.3 [23 34 29 3.3 1.7 2.4 [17 N 4 6 165 17
 
−
177 . . . . . . L1709B-1 16 28 35.4 [23 52 19 44.2 7.6 18.3 54 Y 4 6 165 17
 
−
178 . . . . . . L1757-1 16 29 01.9 [19 35 24 . . . . . . 11.0 . . . N 3 6 165 17
 
−
179 . . . . . . L1757-2 16 29 08.5 [19 42 05 . . . . . . 11.0 . . . N 3 6 165 17
 
−
180 . . . . . . L1689A 16 29 10.4 [24 56 03 2.8 1.6 2.1 11 N 2 6 165 17
 
−
181 . . . . . . L1689B2 16 29 11.4 [24 18 43 9.8 3.6 5.9 [14 Y 3 6 165 17
 
−
182 . . . . . . L1709B-2 16 29 49.3 [23 46 22 44.2 7.6 18.3 54 N 4 6 165 17
 
−
183 . . . . . . L1709C-2 16 30 18.0 [23 40 01 44.2 7.6 18.3 54 N 4 6 165 17
 
−
184 . . . . . . L1689B3 16 30 26.5 [24 37 33 9.5 4.7 6.7 81 N 4 6 165 17
 
−
185 . . . . . . L1689B4 16 30 27.0 [24 21 55 7.6 4.4 5.8 [64 Y 4 6 165 17
 
−
186 . . . . . . DC 3387]18 16 30 33.3 [44 54 53 9.5 1.4 3.6 [66 Y 3 A 700 32
 
−
187 . . . . . . L1709C-1 16 30 52.6 [23 33 54 44.2 7.6 18.3 54 N 4 6 165 17
 
−
188 . . . . . . L1689B5 16 30 55.8 [24 28 16 . . . . . . 17.4 . . . Y 3 6 165 17
 
−
189 . . . . . . L43F 16 31 03.9 [15 45 31 21.8 1.9 6.4 64 N 3 6 165 17
 
−
190 . . . . . . L43D 16 31 28.8 [15 42 54 21.8 1.9 6.4 64 Y 3 6 165 17
 
−
191 . . . . . . L1689B1 16 31 35.2 [24 29 47 . . . . . . 17.4 . . . Y 4 6 165 17
 
−
192 . . . . . . L43E 16 31 47.7 [15 40 51 21.8 1.9 6.4 64 Y 3 6 165 17
 
−
193 . . . . . . DC 3460]78 16 33 34.7 [35 30 27 4.1 2.1 2.9 5 N 4 A 170 16
 
−
194 . . . . . . DC 3464]79 16 34 13.4 [35 08 26 3.8 2.4 3.0 [51 N 4 A 170 16
 
−
195 . . . . . . DC 3463]78 16 34 26.8 [35 21 54 5.9 1.7 3.2 32 N 4 A 170 16
 
−
196 . . . . . . L121 16 36 41.0 [13 59 21 3.1 1.7 2.3 8 N 1 5 165 17
 
−
197 . . . . . . L1782-1 16 39 13.2 [19 36 22 6.0 1.7 3.2 [40 N 1 6 165 17
 
−
240
 
−
TABLE 2ÈContinued
 
−
a b R PA Distance
 
−
Number Source R.A. (1950) Decl. (1950) (arcmin) (arcmin) (arcmin) (deg) EYSO DC Class (pc) References
 
−
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
 
−
198 . . . . . . L1782-2 16 39 36.4 [19 38 00 3.8 2.7 3.2 35 N 2 6 165 17
 
−
199 . . . . . . DC 3393-03 16 42 30.0 [45 54 54 4.3 1.4 2.5 [87 N 4 A 700 32
 
−
200 . . . . . . DC 3405]05 16 43 05.8 [44 26 04 7.1 2.5 4.2 62 N 4 A 700 32
 
−
201 . . . . . . L158-2 16 44 02.6 [13 53 26 8.2 4.1 5.8 55 N 2 6 165 17
 
−
202 . . . . . . L204C-1 16 44 30.6 [12 14 14 5.7 2.2 3.5 1 N 3 6 165 17
 
−
203 . . . . . . L260 16 44 32.5 [09 29 58 7.6 4.1 5.6 [73 Y 2 6 165 17
 
−
204 . . . . . . L204C-2 16 44 58.5 [12 18 04 3.6 1.6 2.4 [5 N 3 6 165 17
 
−
205 . . . . . . L191-1 16 44 59.6 [12 34 43 6.0 2.5 3.9 [52 N 2 5 165 17
 
−
206 . . . . . . L191-2 16 45 01.7 [12 47 38 1.7 1.4 1.5 58 N 1 5 165 17
 
−
207 . . . . . . L255-1 16 45 01.9 [09 48 32 6.3 4.0 5.0 54 Y 3 6 165 17
 
−
208 . . . . . . L234E1 16 45 22.6 [10 52 10 11.7 0.9 3.2 2 N 3 3 165 17
 
−
209 . . . . . . L234E2 16 45 23.2 [10 46 37 11.7 0.9 3.2 2 Y 2 3 165 17
 
−
210 . . . . . . L255-2 16 45 30.9 [09 58 47 4.9 1.9 3.1 [5 N 2 6 165 17
 
−
211 . . . . . . L158-3 16 45 33.9 [14 03 18 7.9 4.1 5.7 54 Y 3 6 165 17
 
−
212 . . . . . . L234E3 16 45 49.0 [10 45 45 3.3 2.1 2.6 56 N 2 3 165 17
 
−
213 . . . . . . L158-4 16 46 22.0 [14 05 23 7.0 3.5 4.9 81 Y 2 6 165 17
 
−
214 . . . . . . L162-1 16 46 22.3 [14 05 33 . . . . . . 7.6 . . . Y 1 6 165 17
 
−
215 . . . . . . L63-4 16 46 49.1 [17 49 47 3.2 1.6 2.3 [49 N 1 6 165 17
 
−
216 . . . . . . L63-3 16 47 10.5 [17 53 51 5.2 1.4 2.7 [25 N 1 6 165 17
 
−
217 . . . . . . L63-2 16 47 11.2 [17 59 52 5.9 3.6 4.6 [82 N 1 6 165 17
 
−
218 . . . . . . L63-1 16 47 20.5 [18 00 53 5.9 3.6 4.6 [82 N 1 6 165 17
 
−
219 . . . . . . L141-2 16 48 03.1 [15 16 54 . . . . . . 6.8 . . . N 2 5 165 17
 
−
220 . . . . . . L141-3 16 48 11.1 [15 12 04 6.9 1.9 3.6 54 N 2 5 165 17
 
−
221 . . . . . . L129-2 16 51 57.6 [16 21 42 2.5 1.1 1.7 25 N 1 6 165 17
 
−
222 . . . . . . L129-1 16 52 18.4 [16 17 10 3.5 1.6 2.4 [79 N 1 6 165 17
 
−
223 . . . . . . L122 16 52 22.4 [16 42 03 3.0 2.1 2.5 80 N 2 6 165 17
 
−
224 . . . . . . CB 68-3 (L146) 16 53 05.4 [15 52 21 11.4 7.9 9.5 [25 Y 2 5 165 17
 
−
225 . . . . . . CB 68-2 (L146) 16 54 00.0 [15 57 11 2.8 1.3 1.9 [5 N 1 5 165 17
 
−
226 . . . . . . CB 68-1 (L146) 16 54 27.5 [16 04 09 4.1 2.1 2.9 [40 Y 2 5 165 17
 
−
227 . . . . . . DC 3504]44 16 59 40.9 [34 20 44 8.8 6.9 7.8 0 N 1 A 170 16
 
−
228 . . . . . . L111 17 11 59.5 [20 27 15 4.3 1.4 2.5 66 N 1 6 165 17
 
−
229 . . . . . . L100 17 13 07.6 [20 54 04 12.3 4.7 7.6 [21 Y/PM 1 6 165 17
 
−
230 . . . . . . L173 17 14 25.4 [18 27 45 9.5 3.2 5.5 [11 N 1 6 165 17
 
−
231 . . . . . . L1772 17 16 25.8 [26 41 37 9.3 3.6 5.8 53 N 1 6 165 17
 
−
232 . . . . . . L1768 17 16 35.0 [26 52 57 13.0 1.6 4.6 81 N 1 6 165 17
 
−
233 . . . . . . L1773 17 18 08.4 [26 50 46 12.0 4.4 7.3 [45 N 1 6 165 17
 
−
234 . . . . . . L1774 17 19 32.1 [27 02 25 7.9 3.2 5.0 [82 Y 1 6 165 17
 
−
235 . . . . . . B68-1 17 19 36.0 [23 47 13 3.8 2.4 3.0 [48 N 2 . . . 165 17
 
−
236 . . . . . . B68-2 17 20 34.0 [23 37 32 4.3 3.5 3.9 [26 N 2 . . . 165 17
 
−
237 . . . . . . B68-3 17 20 49.4 [23 39 57 8.2 2.5 4.5 45 N 2 . . . 165 17
 
−
238 . . . . . . DC 3463[41 17 22 40.3 [42 37 01 12.6 4.4 7.4 62 PM 1 A . . . . . .
 
−
239 . . . . . . DC 3479[44 17 28 52.7 [41 32 37 . . . . . . 3.6 . . . N 2 A . . . . . .
 
−
240 . . . . . . L425 17 44 15.4 [04 34 07 . . . . . . 6.6 . . . Y 1 5 . . . . . .
 
−
241 . . . . . . DC 3475[80 17 44 26.1 [43 42 02 5.2 2.5 3.6 [81 N 1 A . . . . . .
 
−
242 . . . . . . L392 17 50 24.3 [08 26 43 6.5 2.7 4.2 33 N 1 5 200 18
 
−
243 . . . . . . L421 17 51 38.9 [05 46 02 1.6 1.6 1.6 0 N 1 5 200 18
 
−
244 . . . . . . L460 17 55 24.4 [03 46 24 7.6 3.2 4.9 [52 N 1 6 200 18
 
−
245 . . . . . . L432 17 55 46.2 [05 43 45 10.1 3.2 5.7 [8 N 1 6 200 18
 
−
246 . . . . . . L468 17 57 38.0 [03 30 03 4.7 2.1 3.1 0 N 1 5 200 18
 
−
247 . . . . . . L462-1 18 04 51.9 [04 43 57 4.9 2.1 3.2 90 N 1 6 200 18
 
−
248 . . . . . . L462-2 18 04 56.9 [04 40 57 4.9 3.2 4.0 81 N 1 6 200 18
 
−
249 . . . . . . L108 18 07 08.0 [28 18 41 2.8 1.4 2.0 [11 N 3 6 . . . . . .
 
−
250 . . . . . . L422 18 09 20.0 [08 04 46 4.2 1.6 2.6 [36 N 2 6 . . . . . .
 
−
251 . . . . . . L438 18 11 23.8 [07 10 01 3.2 1.7 2.3 [49 N 1 6 . . . . . .
 
−
252 . . . . . . L436 18 11 53.0 [07 23 49 4.6 2.2 3.2 85 N 1 6 . . . . . .
 
−
253 . . . . . . L323 (CB 125) 18 12 39.1 [18 11 47 . . . . . . 10.4 . . . Y 2 6 200 8
 
−
254 . . . . . . L490 18 12 42.5 [03 47 11 3.3 2.2 2.7 [48 N 1 6 200 18
 
−
255 . . . . . . L492 18 13 11.6 [03 47 17 3.8 2.7 3.2 [18 N 1 6 200 18
 
−
256 . . . . . . CB 130-2 (L507) 18 13 37.5 [02 24 28 2.2 1.4 1.8 16 N 3 5 200 18
 
−
257 . . . . . . CB 130-1 (L507) 18 13 39.2 [02 34 06 3.1 1.4 2.1 [88 N 3 5 200 18
 
−
258 . . . . . . CB 130-3 (L507) 18 13 41.5 [02 17 47 3.0 1.3 2.0 61 N 3 5 200 18
 
−
259 . . . . . . L328 18 14 05.3 [18 03 10 1.7 1.4 1.5 47 N 1 6 200 8
 
−
260 . . . . . . L429-1 18 14 28.2 [08 14 40 21.5 8.8 13.8 42 N 2 6 200 18
 
−
261 . . . . . . L429-2 18 14 32.8 [08 19 02 21.5 8.8 13.8 42 N 2 6 200 18
 
−
262 . . . . . . L429-3 18 14 50.8 [08 15 17 21.5 8.8 13.8 42 N 2 6 200 18
 
−
263 . . . . . . L483-1 18 14 54.8 [04 40 23 . . . . . . 11.4 . . . Y 1 6 200 18
 
−
241
 
−
TABLE 2ÈContinued
 
−
a b R PA Distance
 
−
Number Source R.A. (1950) Decl. (1950) (arcmin) (arcmin) (arcmin) (deg) EYSO DC Class (pc) References
 
−
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
 
−
264 . . . . . . L429-4 18 15 05.2 [08 10 07 21.5 8.8 13.8 42 N 2 6 200 18
 
−
265 . . . . . . L483-2 18 15 26.5 [04 34 24 7.4 4.4 5.7 51 N 1 6 200 18
 
−
266 . . . . . . L466 18 17 04.5 [06 07 36 6.3 5.1 5.7 45 N 1 6 200 18
 
−
267 . . . . . . L451 18 19 12.3 [07 14 11 6.8 2.8 4.4 74 N 1 5 200 18
 
−
268 . . . . . . L539-1 18 21 05.7 [01 04 28 . . . . . . 9.4 . . . N 1 6 200 18
 
−
269 . . . . . . L539-2 18 21 46.5 [01 01 05 . . . . . . 5.2 . . . N 1 6 200 18
 
−
270 . . . . . . L416 18 22 46.2 [10 41 26 . . . . . . 3.4 . . . N 3 6 200 18
 
−
271 . . . . . . L406 18 22 50.5 [11 49 11 10.1 7.6 8.8 26 Y 3 5 200 18
 
−
272 . . . . . . L423 18 25 03.9 [10 16 08 7.9 1.9 3.9 [82 N 1 5 200 18
 
−
273 . . . . . . L411 18 25 07.9 [11 29 15 3.0 0.8 1.5 34 N 3 5 200 18
 
−
274 . . . . . . L503 18 26 49.5 [04 40 45 . . . . . . 7.0 . . . N 2 6 200 18
 
−
275 . . . . . . L443-1 18 29 47.1 [08 59 13 4.1 2.8 3.4 14 N 3 5 200 18
 
−
276 . . . . . . L443-2 18 30 01.6 [09 14 41 5.2 4.6 4.9 [37 N 3 5 200 18
 
−
277 . . . . . . L239 18 30 11.5 [26 04 16 3.0 2.4 2.7 [58 N 1 6 . . . . . .
 
−
278 . . . . . . L443-3 18 30 12.0 [09 16 52 5.2 4.6 4.9 [37 N 2 5 200 18
 
−
279 . . . . . . L588-2 18 32 47.0 [00 43 53 . . . . . . 3.8 . . . N 3 6 200 18
 
−
280 . . . . . . L588-3 18 33 18.2 [00 33 25 2.4 1.3 1.8 61 N 3 6 200 18
 
−
281 . . . . . . L588-4 18 33 39.2 [00 40 38 1.1 0.6 0.8 78 N 3 6 200 18
 
−
282 . . . . . . L495 18 36 32.6 [06 41 06 4.9 2.4 3.4 86 N 1 6 200 18
 
−
283 . . . . . . L648-1 18 37 09.7 12 38 37 . . . . . . 6.4 . . . N 4 6 . . . . . .
 
−
284 . . . . . . L648-2 18 37 20.5 12 47 05 . . . . . . 6.4 . . . N 4 6 . . . . . .
 
−
285 . . . . . . L530D-3 18 46 48.0 [05 03 12 6.6 4.0 5.1 11 N 1 6 350 19
 
−
286 . . . . . . L530D-1 18 47 20.5 [04 51 55 16.1 6.9 10.5 5 N 1 6 350 19
 
−
287 . . . . . . L530D-2 18 47 22.1 [04 43 25 16.1 6.9 10.5 5 N 1 6 350 19
 
−
288 . . . . . . L549 18 59 29.8 [05 23 08 3.6 2.2 2.8 79 N 1 5 200 18
 
−
289 . . . . . . L567 19 01 30.2 [04 30 09 10.1 1.9 4.4 51 N 1 6 200 18
 
−
290 . . . . . . B133 (CB 180) 19 03 37.9 [06 59 05 10.7 4.4 6.9 [43 Y 1 6 200 18
 
−
291 . . . . . . L581 19 04 55.5 [03 59 32 19.6 13.9 16.5 34 N 1 6 200 18
 
−
292 . . . . . . L709 19 11 37.3 16 22 01 1.9 1.9 1.9 0 N 4 6 300 18
 
−
293 . . . . . . DC 13[205 19 13 12.4 [36 42 20 4.6 2.2 3.2 [76 N 3 A 130 20
 
−
294 . . . . . . L763 19 16 45.9 23 21 45 7.6 1.1 2.9 11 N 4 6 250 21
 
−
295 . . . . . . L730-1 19 17 40.5 19 51 09 6.8 1.7 3.4 25 N 2 5 160 22
 
−
296 . . . . . . L655 19 17 47.2 08 23 33 3.2 1.2 2.0 [26 N 4 5 200 18
 
−
297 . . . . . . L673-1 19 17 54.7 11 30 36 2.1 1.7 1.9 [32 Y 3 6 300 23
 
−
298 . . . . . . L730-2 19 18 12.4 19 56 53 2.8 1.1 1.8 66 N 2 5 160 22
 
−
299 . . . . . . L673-12 19 18 39.2 10 48 15 . . . . . . 7.6 . . . Y 3 6 300 23
 
−
300 . . . . . . L771 19 18 46.3 23 25 13 2.8 1.4 2.0 51 Y 4 6 400 18
 
−
301 . . . . . . L673-4 19 18 47.1 11 20 11 3.8 0.8 1.7 55 N 3 6 300 23
 
−
302 . . . . . . L673-5 19 18 53.6 11 27 16 2.7 1.1 1.7 [35 N 3 6 300 23
 
−
303 . . . . . . L673-13 19 19 00.9 10 46 45 . . . . . . 7.6 . . . Y 3 6 300 23
 
−
304 . . . . . . L673-14 19 19 01.9 10 51 27 . . . . . . 7.6 . . . Y 3 6 300 23
 
−
305 . . . . . . L673-6 19 19 06.2 11 30 39 1.6 0.8 1.1 47 N 3 6 300 23
 
−
306 . . . . . . L673-7 19 19 14.3 11 15 30 . . . . . . 7.0 . . . N 4 6 300 23
 
−
307 . . . . . . L673-8 19 19 15.4 11 12 20 . . . . . . 7.0 . . . N 4 6 300 23
 
−
308 . . . . . . L684 19 19 16.1 12 23 25 10.4 5.2 7.4 20 N 2 5 300 18
 
−
309 . . . . . . L673-9 19 19 21.1 11 10 54 . . . . . . 7.0 . . . N 4 6 300 23
 
−
310 . . . . . . L673-10 19 19 32.5 11 14 21 2.2 0.9 1.4 60 N 4 6 300 23
 
−
311 . . . . . . L677-1 19 19 50.0 11 27 19 1.6 0.8 1.1 83 N 3 6 300 23
 
−
312 . . . . . . L677-2 19 19 52.8 11 30 46 3.1 0.6 1.4 [37 N 3 6 300 23
 
−
313 . . . . . . L677-3 19 20 07.5 11 15 30 3.6 1.3 2.2 74 N 3 6 300 23
 
−
314 . . . . . . L677-4 19 20 22.8 11 16 57 1.7 0.8 1.2 83 N 3 6 300 23
 
−
315 . . . . . . L774-1 19 20 44.9 23 19 21 2.5 1.9 2.2 25 N 4 5 200 7
 
−
316 . . . . . . L774-2 19 21 34.2 23 17 18 1.0 1.0 1.0 0 N 4 5 200 7
 
−
317 . . . . . . L769-1 19 21 44.8 23 01 48 . . . . . . 9.4 . . . Y 4 6 200 7
 
−
318 . . . . . . L769-2 19 21 50.4 22 53 23 . . . . . . 6.8 . . . Y 4 6 200 7
 
−
319 . . . . . . L769-3 19 22 21.0 23 02 00 . . . . . . 5.4 . . . Y 4 6 200 7
 
−
320 . . . . . . L769-4 19 22 47.0 22 56 36 . . . . . . 6.2 . . . N 4 6 200 7
 
−
321 . . . . . . L698 19 23 37.5 12 59 48 11.0 1.1 3.5 [2 N 3 6 300 18
 
−
322 . . . . . . L778-1 19 24 19.8 23 53 04 19.6 0.9 4.2 [48 Y 4 6 200 7
 
−
323 . . . . . . L778-2 19 25 22.0 23 39 45 19.6 0.9 4.2 [48 N 4 6 200 7
 
−
324 . . . . . . L778-3 19 25 54.8 23 37 14 19.6 0.9 4.2 [48 N 4 6 200 7
 
−
325 . . . . . . L778-4 19 26 02.6 23 51 12 1.3 1.3 1.3 0 N 4 6 200 7
 
−
326 . . . . . . B335 19 34 35.6 07 27 34 3.2 2.1 2.6 14 Y 4 . . . 250 24
 
−
327 . . . . . . L694-1 19 38 06.5 10 43 33 8.2 2.5 4.5 82 N 4 6 . . . . . .
 
−
328 . . . . . . L694-2 19 38 42.4 10 49 59 . . . . . . 6.4 . . . N 4 6 . . . . . .
 
−
329 . . . . . . L694-3 19 38 54.0 10 43 42 2.4 1.7 2.0 [12 N 4 6 . . . . . .
 
−
242
 
−
TABLE 2ÈContinued
 
−
a b R PA Distance
 
−
Number Source R.A. (1950) Decl. (1950) (arcmin) (arcmin) (arcmin) (deg) EYSO DC Class (pc) References
 
−
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
 
−
330 . . . . . . L758 19 44 12.8 18 54 47 1.6 0.9 1.2 51 N 4 5 400 18
 
−
331 . . . . . . L880 20 11 49.4 40 03 59 7.4 5.7 6.5 [35 N 4 5 700 18
 
−
332 . . . . . . L1152 20 35 26.0 67 43 23 1.6 0.6 1.0 57 Y 1 5 325 25
 
−
333 . . . . . . L1041-1 20 36 05.5 57 33 36 1.7 0.9 1.2 32 Y 1 5 440 23
 
−
334 . . . . . . L1041-2 20 36 05.9 57 38 48 1.8 0.8 1.2 30 N 1 5 440 23
 
−
335 . . . . . . L922-1 20 36 46.5 44 21 24 . . . . . . 2.6 . . . N 4 6 700 18
 
−
336 . . . . . . L922-2 20 37 04.6 44 25 20 . . . . . . 1.8 . . . N 4 6 700 18
 
−
337 . . . . . . L917 20 38 16.6 43 58 37 3.2 0.9 1.7 44 N 3 6 . . . . . .
 
−
338 . . . . . . L918 20 39 02.5 43 54 57 4.9 1.7 2.9 64 N 3 6 . . . . . .
 
−
339 . . . . . . L1049-1 20 39 50.8 57 16 45 3.0 1.4 2.0 50 N 2 6 440 23
 
−
340 . . . . . . L1147 20 39 58.4 67 09 36 6.5 1.3 2.9 44 N 2 3 325 25
 
−
341 . . . . . . L1049-2 20 40 16.8 57 22 57 1.9 0.8 1.2 9 N 3 4 440 23
 
−
342 . . . . . . L896-2 20 40 26.3 39 36 01 . . . . . . 3.0 . . . N 4 5 . . . . . .
 
−
343 . . . . . . L896-1 20 40 28.8 39 42 22 7.4 4.0 5.4 62 N 4 5 . . . . . .
 
−
344 . . . . . . L1148 20 40 38.7 67 09 48 7.1 1.6 3.4 46 N 2 6 325 25
 
−
345 . . . . . . L1155C 20 43 00.0 67 41 47 4.6 3.2 3.8 55 N 2 6 325 25
 
−
346 . . . . . . L1155D 20 43 17.9 67 26 12 4.9 1.4 2.6 43 N 1 6 325 25
 
−
347 . . . . . . L915 20 43 23.0 42 58 52 6.1 3.0 4.3 33 N 4 6 . . . . . .
 
−
348 . . . . . . L1155E 20 43 46.3 67 31 02 2.8 1.4 2.0 32 N 1 6 325 25
 
−
349 . . . . . . L1082C-3 20 47 59.4 60 00 36 4.4 0.6 1.6 47 N 3 5 440 26
 
−
350 . . . . . . L1082C-2 20 48 38.9 60 04 25 2.2 0.6 1.1 49 N 3 5 440 26
 
−
351 . . . . . . L1082C-1 20 50 20.0 60 07 13 2.5 1.7 2.1 43 Y 2 5 440 26
 
−
352 . . . . . . L1082B 20 52 40.7 59 59 59 . . . . . . 8.2 . . . Y 3 5 440 26
 
−
353 . . . . . . L981-1 20 58 36.3 50 08 19 . . . . . . 8.2 . . . N 3 6 700 27
 
−
354 . . . . . . L981-2 20 58 38.0 50 05 09 . . . . . . 8.2 . . . N 3 6 700 27
 
−
355 . . . . . . L971-1 20 59 08.1 49 17 21 2.4 1.1 1.6 24 N 2 5 700 27
 
−
356 . . . . . . L971-2 20 59 15.8 49 07 34 3.0 1.4 2.0 [3 N 2 5 700 27
 
−
357 . . . . . . L981-3 20 59 22.3 50 09 41 . . . . . . 8.2 . . . Y 3 6 700 27
 
−
358 . . . . . . L1174 20 59 22.7 68 01 12 4.7 2.2 3.2 63 Y 2 4 288 25
 
−
359 . . . . . . L1172A-2 21 01 10.8 67 34 34 5.1 3.5 4.2 12 N 1 6 288 25
 
−
360 . . . . . . L1172A-1 21 01 39.6 67 41 59 1.9 1.1 1.4 [34 Y 1 6 288 25
 
−
361 . . . . . . L1172A-3 21 03 22.6 67 29 06 2.5 1.3 1.8 1 N 1 6 288 25
 
−
362 . . . . . . L1063 21 06 44.6 56 06 09 4.4 1.7 2.7 50 N 3 5 800 18
 
−
363 . . . . . . B361-1 21 10 41.7 47 12 05 11.1 11.1 11.1 0 Y 3 . . . 350 28
 
−
364 . . . . . . B361-2 21 10 53.2 47 07 23 11.1 11.1 11.1 0 Y 3 . . . 350 28
 
−
365 . . . . . . L1125-1 21 13 07.8 61 32 26 3.2 1.5 2.2 72 N 2 5 300 1
 
−
366 . . . . . . L1125-2 21 14 07.0 61 27 10 . . . . . . 4.8 . . . Y 2 5 300 1
 
−
367 . . . . . . L944-1 21 14 42.6 42 59 47 3.0 0.8 1.5 [49 N 4 6 . . . . . .
 
−
368 . . . . . . L944-2 21 15 54.0 43 05 41 . . . . . . 2.8 . . . N 4 6 . . . . . .
 
−
369 . . . . . . L944-3 21 16 59.7 43 12 57 0.9 0.6 0.7 27 N 4 6 . . . . . .
 
−
370 . . . . . . L952-1 21 18 08.5 43 18 07 2.0 0.7 1.2 44 N 4 5 . . . . . .
 
−
371 . . . . . . L952-2 21 18 25.0 43 19 59 3.2 0.8 1.6 64 N 4 5 . . . . . .
 
−
372 . . . . . . L953 21 19 31.8 43 08 46 0.9 0.5 0.7 [19 N 4 6 . . . . . .
 
−
373 . . . . . . L1021 21 20 34.8 50 50 17 0.7 0.6 0.6 0 N 4 6 200 29
 
−
374 . . . . . . L1014-1 21 22 20.6 49 56 52 7.0 3.2 4.7 67 N 4 6 200 29
 
−
375 . . . . . . L1014-2 21 22 22.2 49 46 10 2.4 1.1 1.6 [58 N 3 6 200 29
 
−
376 . . . . . . L1099-1 21 34 27.9 57 13 18 1.7 0.8 1.2 81 N 4 5 . . . . . .
 
−
377 . . . . . . L973 21 35 16.3 43 06 57 2.2 0.9 1.4 [8 Y 3 5 . . . . . .
 
−
378 . . . . . . L1111 21 38 53.6 57 34 24 3.7 2.4 3.0 [42 N 4 6 150 29
 
−
379 . . . . . . L1121 21 39 10.0 58 02 33 2.4 1.7 2.0 25 Y 4 5 . . . . . .
 
−
380 . . . . . . L1103-1 21 39 49.8 56 23 32 4.4 2.4 3.2 54 N 4 6 . . . . . .
 
−
381 . . . . . . L1103-2 21 40 41.0 56 30 07 2.1 1.0 1.4 21 N 4 6 150 29
 
−
382 . . . . . . L1113-2 21 42 45.4 56 57 33 2.4 1.6 2.0 64 N 4 5 150 29
 
−
383 . . . . . . L1113-1 21 42 56.7 56 56 25 0.9 0.9 0.9 0 N 4 5 150 29
 
−
384 . . . . . . L1031C 21 44 35.9 47 03 42 7.3 2.8 4.5 [87 Y 3 5 900 30
 
−
385 . . . . . . L1139-1 21 53 14.7 58 20 59 2.1 0.9 1.4 [48 N 2 5 . . . . . .
 
−
386 . . . . . . L1139-2 21 53 47.3 58 20 14 4.6 1.1 2.2 55 Y 2 5 . . . . . .
 
−
387 . . . . . . L1143 21 57 03.0 58 42 25 7.3 2.1 3.9 46 Y 4 6 . . . . . .
 
−
388 . . . . . . L1166 22 03 46.7 59 19 07 1.9 0.9 1.3 59 N 4 6 . . . . . .
 
−
389 . . . . . . L1164 22 05 07.7 58 51 15 . . . . . . 7.4 . . . Y 4 6 . . . . . .
 
−
390 . . . . . . L1235 22 14 44.4 73 08 05 6.3 3.5 4.7 67 N 2 6 200 3
 
−
391 . . . . . . L1195 22 25 18.1 61 01 06 4.6 1.9 3.0 13 N 2 5 . . . . . .
 
−
392 . . . . . . L1221 22 26 38.4 68 45 48 6.2 2.4 3.9 43 Y 2 5 200 23
 
−
393 . . . . . . L1251A-2 22 26 46.5 74 58 10 3.3 2.2 2.7 54 N 3 5 300 31
 
−
394 . . . . . . L1185 22 27 27.6 58 53 30 4.1 1.6 2.6 75 N 3 6 . . . . . .
 
−
395 . . . . . . L1251A-1 22 30 00.8 74 57 04 8.2 5.1 6.5 [67 Y 2 5 300 31
 
−
243
 
−
200 400 600 800 1000
 
−
5000
 
−
5500
 
−
6000
 
−
6500
 
−
7000
 
−
0 1 2 3 4 5
 
−
0
 
−
0.2
 
−
0.4 Lynds 5
 
−
0
 
−
0.2
 
−
0.4 Lynds 6
 
−
0
 
−
0.2
 
−
0.4 Hartley A
 
−
244 LEE & MYERS
 
−
TABLE 2ÈContinued
 
−
a b R PA Distance
 
−
Number Source R.A. (1950) Decl. (1950) (arcmin) (arcmin) (arcmin) (deg) EYSO DC Class (pc) References
 
−
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
 
−
396 . . . . . . L1197 22 35 08.0 58 41 46 4.3 1.2 2.3 [56 N 4 6 . . . . . .
 
−
397 . . . . . . L1251 22 36 26.0 74 54 46 7.1 1.9 3.7 52 N 1 5 300 31
 
−
398 . . . . . . L1229 23 12 16.8 61 46 47 3.8 1.4 2.3 24 N 4 5 . . . . . .
 
−
399 . . . . . . L1234 23 15 47.5 62 10 15 1.9 0.8 1.2 [73 N 4 6 . . . . . .
 
−
400 . . . . . . CB 243 (L1246) 23 23 07.2 63 19 48 3.3 1.1 1.9 [73 Y 4 6 . . . . . .
 
−
401 . . . . . . L1262A (CB 244) 23 23 47.7 74 01 29 4.7 2.1 3.1 [73 Y 2 6 200 3
 
−
402 . . . . . . CB 246 (L1253) 23 54 10.8 58 17 29 3.2 2.1 2.6 [48 N 3 6 140 3
 
−
403 . . . . . . L1263 23 54 54.2 64 32 27 2.5 1.3 1.8 [10 N 1 5 . . . . . .
 
−
404 . . . . . . L1271-1 23 57 32.6 67 05 07 11.4 1.1 3.5 55 N 4 5 . . . . . .
 
−
405 . . . . . . L1271-2 23 58 20.7 66 52 29 2.1 1.1 1.5 31 Y 4 5 . . . . . .
 
−
406 . . . . . . L1271-3 23 59 15.3 67 01 48 2.8 2.2 2.5 [51 N 4 5 . . . . . .
 
−
NOTES.ÈThese 406 sources are positions showing local intensity minima in the STScI Digitized Sky Survey (DSS). Cols. (1)È(4) : Sequential numbers,
 
−
source names, and their coordinates. Cols. (5) and (6) : a and b are sizes of major and minor axis of FWHM of selected cores, respectively. Col. (7) : Geometric
 
−
mean (ab)0.5 for the cores whose a and b are measured, or the equivalent diameter 2](A/n)0.5 for the cores in which a and b are not measured owing to its
 
−
irregularity. Col. (8) : Position angle of the core. Col. (9) : N, starless cores ; Y, cores with embedded YSOs; PM, cores with preÈmain-sequence (PMS) stars ;
 
−
and PM*, PMSs that are determined by optical spectroscopy (Herbig & Bell 1988). Col. (10) : Darkness contrast of the opaque core to the background, where
 
−
1 corresponds to the least dark and 4 to the most dark. Col. (11) : Lynds opacity class and Hartley A class. Col. (12) : Distances to the cores. Col. (13) :
 
−
References for core distances.
 
−
REFERENCES.È(1) Lindblad et al. 1973, Lindblad ring ; (2) Herbig & Jones 1983, Per OB2; (3) Snell 1981; (4) Elias 1978b, Taurus; (5) Maddalena et al. 1986,
 
−
Orion A, B; (6) Murdin & Penston 1977; (7) Goodman et al. 1993; (8) Bok & McCarthy 1974; (9) Carballo & Sahu 1994; (10) Harjunpaa, Lijiestrom, &
 
−
Mattila 1991, Vela; (11) Schwartz 1991, Cha I ; (12) Rogers 1960, Coal Sack; (13) Hetem et al. 1988, Musca; (14) Gauvin & Strom 1992, Cha II, III ; (15)
 
−
Neckel & Klare 1980, G317-4; (16) Murphy 1985, Lupus; (17) Chini 1981, Ophiuchus; (18) Dame & Thaddeus 1985, Aquila Rift (200 pc), Cloud B (300 pc),
 
−
Cloud C (500 pc), Vul Rift (400 pc), Cyg Rift (700 pc), Cyg OB7 (800 pc) ; (19) Beichman et al. 1986; (20) Marraco & Rydgren 1981; (21) Cohen & Kuhi 1979;
 
−
(22) Frerking & Langer 1982; (23) Felli, Palagi, & Tofani 1992; (24) Tomita, Saito, & Ohtani 1979; (25) Straizys et al. 1992; (26) Viotti 1969; (27) Clark 1986;
 
−
(28) Schmidt 1975; (29) Leung, Kutner, &Mead 1982; (30) Elias 1978a; (31) Kun & Prusti 1993; (32) Graham & Frogel 1985, Norma.
 
−
4@ with a mean (^s.e.m.) of 3.@7(^0.1). This distribution is
 
−
similar to that found by previous study of CB. The size
 
−
distribution of starless cores, which comprise a majority,
 
−
resembles the size distribution of all cores, while the size of
 
−
cores with EYSOs is uniformly distributed between 1@ and
 
−
8@. The interesting thing is that the mean size (5.@1^0.@4) of
 
−
the cores with EYSOs is larger than that (3.@3^0.@1) of starless
 
−
cores.
 
−
We also Ðnd a corresponding di†erence in the distribution
 
−
of the linear sizes, as illustrated in Figure 5. Distances
 
−
(Table 2, col. [12]) of cores for determination of the linear
 
−
sizes have been obtained from numerous papers (see refer-
 
−
FIG. 2.ÈExample of a cut-proÐle of L1622 cloud. This cut-proÐle was
 
−
obtained by crossing two intensity minima of L1622A and L1622B. The
 
−
angular size for 1 pixel in the abscissa is about 0A.6. The data value (DN) is
 
−
on a scale of photographic density (c) in the expression of c\DN/6553.4
 
−
(Postman 1996). The data values (IB and IC) of DSS for the background
 
−
and the core are approximately adopted from this proÐle.
 
−
ences listed in Table 2) referred to by Dame et al. (1987),
 
−
BM, Vilas-Boas et al. (1994), Hilton & Lahulla (1995), and
 
−
Chen et al. (1997). We adopted the distances given by those
 
−
papers if our sources are in a vicinity (within 1¡) of the
 
−
FIG. 3.ÈRelation of the darkness contrast (DC) to Lynds class 5 and 6
 
−
and HMSTG class A. Lynds 6 and HMSTG A clouds more likely have a
 
−
DC of 3 or 4 than Lynds 5 clouds.
 
−
TABLE 3
 
−
IRAS POINT SOURCES AND PMS STARS ASSOCIATED WITH OPTICALLY SELECTED CORES
 
−
F12km F25km F60km F100km Core Name IRAS or PMSa Name R.A. (1950) Decl. (1950) (Jy) (Jy) (Jy) (Jy)
 
−
L1358-1 . . . . . . . . . . . . . . . . . . 02514]6902 02 51 24.0 69 02 36 0.76 0.25L 0.40L 6.61
 
−
CB 17 . . . . . . . . . . . . . . . . . . . . 04005]5647 04 00 30.8 56 47 59 0.44L 0.25L 0.90 5.81
 
−
L1495-3 . . . . . . . . . . . . . . . . . . 04154]2823 04 15 25.7 28 23 56 0.45 1.02 1.96 7.80L
 
−
L1506A . . . . . . . . . . . . . . . . . . 04207]2449 04 20 39.0 24 49 24 0.46 0.65 0.86 1.92
 
−
B217-1 . . . . . . . . . . . . . . . . . . . 04249]2612 04 24 53.2 26 12 39 0.36L 1.33 4.61 9.29
 
−
L1524-2 . . . . . . . . . . . . . . . . . . 04264]2426 04 26 21.7 24 26 26 14.86 38.73 59.70 47.42
 
−
L1524-1 . . . . . . . . . . . . . . . . . . 04265]2433 04 26 28.0 24 33 23 0.44 2.91 5.40 9.12L
 
−
L1524-3 . . . . . . . . . . . . . . . . . . 04264]2426 04 26 21.7 24 26 26 14.86 38.73 59.70 47.42
 
−
TMC 2-2 . . . . . . . . . . . . . . . . . 04288]2417 04 28 48.7 24 17 54 0.33 1.03 2.56 5.70
 
−
TMC 2A . . . . . . . . . . . . . . . . . 04292]2422 04 29 13.2 24 22 39 1.06 3.98 7.18 9.82
 
−
TMC 2-1 . . . . . . . . . . . . . . . . . 04292]2422 04 29 13.2 24 22 39 1.06 3.98 7.18 9.82
 
−
B18-4 . . . . . . . . . . . . . . . . . . . . . 04325]2402 04 32 31.6 24 02 08 0.25L 2.11 12.82 22.28
 
−
L1527A-1 . . . . . . . . . . . . . . . . 04354]2604 04 35 23.9 26 04 51 1.91 3.87 5.92 6.49
 
−
L1534 . . . . . . . . . . . . . . . . . . . . 04363]2539 04 36 16.2 25 39 07 0.55 0.72 0.40L 2.01L
 
−
L1534 . . . . . . . . . . . . . . . . . . . . 04365]2535 04 36 31.0 25 35 52 1.19 8.63 35.97 39.08
 
−
L1534 . . . . . . . . . . . . . . . . . . . . 04369]2539 04 36 54.6 25 39 17 5.01 6.79 7.24 18.20
 
−
TMC 1-1 . . . . . . . . . . . . . . . . . 04381]2540 04 38 07.6 25 40 48 0.44 2.68 10.28 13.93
 
−
TMC 1C . . . . . . . . . . . . . . . . . 04386]2550 04 38 34.2 25 50 43 0.54 1.54 2.88 8.02L
 
−
B25A . . . . . . . . . . . . . . . . . . . . . 05418]0907 05 41 45.3 09 07 40 0.28 2.91 25.59 74.47
 
−
L1622B . . . . . . . . . . . . . . . . . . . 05523]0146 05 52 17.2 01 46 41 0.34L 0.31 1.45 31.33
 
−
L1645 . . . . . . . . . . . . . . . . . . . . 06053[0533 06 05 16.3 [05 33 49 0.25L 0.60 13.06 22.28
 
−
L1578-1, L1578-2 . . . . . . . Bretz 34 06 05 42.5 18 08 21 . . . . . . . . . . . .
 
−
V14 . . . . . . . . . . . . . . . . . . . . . . . 08077[35561 08 07 40.2 [35 56 07 0.63 3.73 18.20 47.42
 
−
DC 2573[25-1 . . . . . . . . . 08153[3945 08 15 16.6 [39 45 44 0.41 1.24 1.47 17.70L
 
−
DC 2660[75-2 . . . . . . . . . 08196[4931 08 19 37.1 [49 31 13 0.25L 7.05 53.46 74.47L
 
−
DC 2674[75 . . . . . . . . . . . . 08243[5050 08 24 16.5 [50 50 44 0.82 6.31 26.06 58.08
 
−
DC 2672[72 . . . . . . . . . . . . 08251[5030 08 25 03.4 [50 30 34 0.25L 0.25L 1.19 17.06
 
−
DC 2977[28 . . . . . . . . . . . . 11591[64521 11 59 03.1 [64 52 11 0.25L 6.55 77.27 192.31
 
−
Ch 7 . . . . . . . . . . . . . . . . . . . . . . 12496[7650 12 49 38.0 [76 50 45 39.45 85.51 104.71 87.10
 
−
Ch 7 . . . . . . . . . . . . . . . . . . . . . . 12501[7658 12 50 03.0 [76 58 49 0.25L 1.02 2.70 5.35L
 
−
Ch 19-1 . . . . . . . . . . . . . . . . . . 12571[7654 12 57 07.6 [76 54 31 0.31L 0.52 0.86 5.81
 
−
DC 3038[142 . . . . . . . . . . 13037[76442 13 03 41.4 [76 44 03 0.25L 1.05 6.37 22.49
 
−
DC 3148[51 . . . . . . . . . . . . 14451[6502 14 45 07.6 [65 02 55 1.26 1.46 4.66 22.70
 
−
DC 3379]164 . . . . . . . . . . 15363[3436 15 36 15.2 [34 36 32 0.56 0.82 0.40L 13.30L
 
−
DC 3388]165-4 . . . . . . . . 15390[3400 15 39 01.6 [34 00 32 0.25L 0.29L 0.76 6.73
 
−
DC 3388]165-4,5 . . . . . . 15399[33592 15 39 51.2 [33 59 36 0.25L 1.28 15.28 41.30
 
−
DC 3392]161-1 . . . . . . . . 15420[3408 15 42 01.3 [34 08 09 2.58 3.98 7.94 24.43
 
−
DC 3390]150 . . . . . . . . . . 15449[3506 15 44 51.6 [35 06 36 0.91 1.98 1.96 12.47L
 
−
DC 3386]119-2 . . . . . . . . 15534[3740 15 53 24.5 [37 40 34 2.44 4.53 4.97 10.47L
 
−
DC 3397]92-1 . . . . . . . . . 16054[3857 16 05 25.6 [38 57 50 0.60L 0.72 6.08 63.68
 
−
DC 3397]92-1 . . . . . . . . . 16059[3850 16 05 56.2 [38 50 28 0.26L 0.27L 1.18 8.24
 
−
DC 3397]92-1 . . . . . . . . . 16065[3903 16 06 27.6 [39 03 30 0.38 0.54 0.61 24.66L
 
−
DC 3397]92-1,2,3 . . . . . . 16073[3900 16 07 17.0 [39 00 24 0.25L 0.28L 0.84 11.69
 
−
DC 3397]92-2 . . . . . . . . . 16059[3850 16 05 56.2 [38 50 28 0.26L 0.27L 1.18 8.24
 
−
DC 3397]92-2,3 . . . . . . . . 16065[3903 16 06 27.6 [39 03 30 0.38 0.54 0.61 24.66L
 
−
DC 3402]90-1,2,3 . . . . . . 16082[38523 16 08 12.7 [38 52 25 4.92 3.44 0.90 5.01L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16226[2417 16 22 36.0 [24 17 56 4.02 10.28 2.56L 26.55L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16226[2408 16 22 38.7 [24 08 52 2.21 3.05 25.12L 794.33L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16228[2418 16 22 47.9 [24 18 48 1.91 3.05 2.94L 29.92L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16232[2427 16 23 09.6 [24 27 35 3.47L 52.48 469.89L 1018.59
 
−
L1681A . . . . . . . . . . . . . . . . . . 16234[2409 16 23 22.7 [24 09 30 3.44 3.80 2.81L 24.21L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16234[2436 16 23 25.0 [24 36 58 0.91 1.49 8.24 28.31L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16235[2416 16 23 31.5 [24 16 56 34.99 265.46 2187.76 4655.86
 
−
L1681A . . . . . . . . . . . . . . . . . . 16237[2428 16 23 44.2 [24 28 07 2.88 7.80 148.59L 299.23
 
−
L1681A . . . . . . . . . . . . . . . . . . 16239[2428 16 23 53.5 [24 28 12 4.45 19.05 197.70L 787.05L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16239[2438 16 23 56.6 [24 38 52 3.56 6.92 8.47 39.81L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16241[2430 16 24 03.6 [24 30 43 39.45 73.79 197.70 586.14
 
−
L1681A . . . . . . . . . . . . . . . . . . 16243[2422 16 24 15.7 [24 22 06 2.09L 6.55 64.27L 218.78
 
−
L1681A . . . . . . . . . . . . . . . . . . 16244[24321 16 24 26.2 [24 32 53 9.91 67.30 111.69L 349.95
 
−
L1681A . . . . . . . . . . . . . . . . . . 16246[2423 16 24 34.7 [24 23 51 7.80 46.56 65.46L 224.91L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16246[2415 16 24 38.1 [24 15 22 0.93 1.51 6.43L 165.96L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16246[2436 16 24 38.6 [24 36 36 1.63 2.94 4.57 31.05L
 
−
L1681A . . . . . . . . . . . . . . . . . . 16248[2424 16 24 47.7 [24 24 59 5.70 17.22 65.46L 35.65
 
−
L1681A . . . . . . . . . . . . . . . . . . 16253[2429 16 25 20.4 [24 29 55 0.25L 0.42L 2.91 16.29
 
−
L1681A . . . . . . . . . . . . . . . . . . 16257[2421 16 25 43.4 [24 21 50 0.67 0.73 2.07 52.48L
 
−
TABLE 3ÈContinued
 
−
F12km F25km F60km F100km Core Name IRAS or PMSa Name R.A. (1950) Decl. (1950) (Jy) (Jy) (Jy) (Jy)
 
−
L1696B-1 . . . . . . . . . . . . . . . . 16242[2412 16 24 10.2 [24 12 34 2.27 19.77 33.73 165.96L
 
−
L1696B-1 . . . . . . . . . . . . . . . . 16246[2415 16 24 38.1 [24 15 22 0.93 1.51 6.43L 165.96L
 
−
L1696B-1 . . . . . . . . . . . . . . . . 16257[2421 16 25 43.4 [24 21 50 0.67 0.73 2.07 52.48L
 
−
L1709B-1 . . . . . . . . . . . . . . . . 16286[2355 16 28 34.7 [23 55 13 1.19 3.73 9.46 60.81L
 
−
L1709B-1 . . . . . . . . . . . . . . . . 16294[2358 16 29 21.3 [23 58 57 0.25L 0.71L 1.18 15.56
 
−
L1689B2 . . . . . . . . . . . . . . . . . 16293[24221 16 29 20.9 [24 22 13 0.25L 1.82 255.86 1028.02
 
−
L1689B4, L1689B1 . . . . . . 16306[2425 16 30 33.2 [24 25 21 0.37L 0.39L 1.49 31.05
 
−
DC 3387]18 . . . . . . . . . . . . 16307[4455 16 30 39.9 [44 55 13 1.69L 0.62 2.81 38.73L
 
−
L1689B5 . . . . . . . . . . . . . . . . . 16306[2425 16 30 33.2 [24 25 21 0.37L 0.39L 1.49 31.05
 
−
L1689B5 . . . . . . . . . . . . . . . . . 16314[2439 16 31 23.9 [24 39 17 0.25L 0.47L 1.11 15.00
 
−
L43D . . . . . . . . . . . . . . . . . . . . . 16316[1540 16 31 37.7 [15 40 52 1.50 6.03 35.32 64.27
 
−
L1689B1 . . . . . . . . . . . . . . . . . 16314[2439 16 31 23.9 [24 39 17 0.25L 0.47L 1.11 15.00
 
−
L43E . . . . . . . . . . . . . . . . . . . . . 16316[1540 16 31 37.7 [15 40 52 1.50 6.03 35.32 64.27
 
−
L260 . . . . . . . . . . . . . . . . . . . . . . 16442[0930 16 44 14.2 [09 30 03 0.57 3.31 7.80 7.52
 
−
L255-1 . . . . . . . . . . . . . . . . . . . . 16451[0953 16 45 07.0 [09 53 20 0.25L 0.32L 0.60 12.82
 
−
L234E2 . . . . . . . . . . . . . . . . . . . 16452[1046 16 45 10.0 [10 45 53 0.25L 0.34L 0.99 7.11
 
−
L158-3 . . . . . . . . . . . . . . . . . . . . 16455[1405 16 45 32.0 [14 05 31 0.63 0.90 1.22 13.30L
 
−
L158-4 . . . . . . . . . . . . . . . . . . . . 16464[1407 16 46 25.2 [14 07 48 0.60L 0.36L 0.63 6.49
 
−
L162-1 . . . . . . . . . . . . . . . . . . . . 16459[1411 16 45 54.7 [14 11 20 1.41 1.91 2.33L 6.49
 
−
L162-1 . . . . . . . . . . . . . . . . . . . . 16464[1407 16 46 25.2 [14 07 48 0.60L 0.36L 0.63 6.49
 
−
CB 68-3 . . . . . . . . . . . . . . . . . . 16534[1557 16 53 24.6 [15 57 27 0.39 1.41 1.94 12.13L
 
−
CB 68-1 . . . . . . . . . . . . . . . . . . 16545[1604 16 54 27.2 [16 04 48 0.25L 1.49 19.41 33.73
 
−
L100 . . . . . . . . . . . . . . . . . . . . . . 17131[2053 17 13 03.9 [20 53 39 0.38L 1.22L 4.13 14.59
 
−
L100 . . . . . . . . . . . . . . . . . . . . . . 17134[20563 17 13 22.4 [20 56 13 8.95 5.60 0.95 16.75L
 
−
L1774 . . . . . . . . . . . . . . . . . . . . . 17194[2705 17 19 22.9 [27 05 56 0.72L 6.19 6.73 10.86L
 
−
DC 3463-41 . . . . . . . . . . . . . . 17229[42373 17 22 53.4 [42 37 19 1.47 0.79 1.53 17.06
 
−
L425 . . . . . . . . . . . . . . . . . . . . . . 17442[0433 17 44 11.7 [04 33 31 0.41 2.31 8.17 9.64
 
−
L323(CB 125) . . . . . . . . . . . . 18122[1818 18 12 14.2 [18 18 30 3.91 12.13 58.08L 625.17L
 
−
L483-1 . . . . . . . . . . . . . . . . . . . . 18148[04401 18 14 50.6 [04 40 49 0.25L 6.92 88.72 165.96
 
−
L406 . . . . . . . . . . . . . . . . . . . . . . 18231[1144 18 23 04.5 [11 44 50 7.38 10.67 21.68L 440.55L
 
−
L406 . . . . . . . . . . . . . . . . . . . . . . 18233[1154 18 23 15.2 [11 54 22 15.14 88.72 937.56 2857.59
 
−
B133 . . . . . . . . . . . . . . . . . . . . . . 19038[0659 19 03 48.0 [06 59 47 0.25L 0.50 0.98 9.82
 
−
L673-1 . . . . . . . . . . . . . . . . . . . . 19179]1129 19 17 54.0 11 29 56 0.27L 1.06 3.94 18.54
 
−
L673-12 . . . . . . . . . . . . . . . . . . 19184]1055 19 18 24.2 10 55 15 3.73 5.45 3.70L 9.73
 
−
L673-12 . . . . . . . . . . . . . . . . . . 19190]1048 19 19 00.4 10 48 12 1.13 3.40 7.80 61.38L
 
−
L771 . . . . . . . . . . . . . . . . . . . . . . 19187]2325 19 18 39.8 23 25 50 0.25L 0.25L 1.04 6.61
 
−
L673-13 . . . . . . . . . . . . . . . . . . 19190]1048 19 19 00.4 10 48 12 1.13 3.40 7.80 61.38L
 
−
L673-14 . . . . . . . . . . . . . . . . . . 19190]1048 19 19 00.4 10 48 12 1.13 3.40 7.80 61.38L
 
−
L774-1, L769-1 . . . . . . . . . . 19216]2302 19 21 35.9 23 02 54 0.51L 0.26 1.13 7.38L
 
−
L774-1 . . . . . . . . . . . . . . . . . . . . 19219]2300 19 21 54.1 23 00 46 0.25L 0.25L 2.78 12.47
 
−
L774-1 . . . . . . . . . . . . . . . . . . . . 19221]2300 19 22 08.3 23 00 05 0.54 1.22 1.57 5.81L
 
−
L769-2 . . . . . . . . . . . . . . . . . . . . 19221]2300 19 22 08.3 23 00 05 0.54 1.22 1.57 5.81L
 
−
L769-3 . . . . . . . . . . . . . . . . . . . . 19221]2300 19 22 08.3 23 00 05 0.54 1.22 1.57 5.81L
 
−
L778-1 . . . . . . . . . . . . . . . . . . . . 19244]2352 19 24 23.8 23 52 10 0.33L 0.25L 3.05 8.63
 
−
L778-1 . . . . . . . . . . . . . . . . . . . . 19244]2350 19 24 23.9 23 50 56 0.33 0.57 0.40L 9.12
 
−
B335 . . . . . . . . . . . . . . . . . . . . . . 19346]07271 19 34 35.3 07 27 24 0.25L 0.25L 8.32 42.07
 
−
L1152 . . . . . . . . . . . . . . . . . . . . . 20353]6742 20 35 20.1 67 42 30 0.25L 0.34 4.09 7.11
 
−
L1041-1 . . . . . . . . . . . . . . . . . . 20361]5733 20 36 08.7 57 33 40 0.25L 1.16 11.38 26.55
 
−
L1082C-1 . . . . . . . . . . . . . . . . 20503]6006 20 50 19.6 60 06 41 0.25L 0.30 1.54 13.80L
 
−
L1082B . . . . . . . . . . . . . . . . . . . 20521]6003 20 52 04.7 60 03 14 0.49 1.36 2.47 6.25
 
−
L1082B . . . . . . . . . . . . . . . . . . . 20527]5958 20 52 41.0 59 58 21 0.39L 0.25L 1.36 5.65
 
−
L981-3 . . . . . . . . . . . . . . . . . . . . 20595]5009 20 59 32.3 50 09 53 1.15 2.81 6.55 39.81L
 
−
L1174 . . . . . . . . . . . . . . . . . . . . . 20597]6800 20 59 42.1 68 00 13 0.25L 0.82 4.49 54.95L
 
−
L1172A-1 . . . . . . . . . . . . . . . . 21017]6742 21 01 44.2 67 42 24 0.28L 0.26 1.33 5.81
 
−
B361-1,2 . . . . . . . . . . . . . . . . . . 21107]4712 21 10 41.0 47 12 01 0.25L 0.78 15.70 39.08
 
−
L1125-2 . . . . . . . . . . . . . . . . . . 21137]6126 21 13 44.5 61 26 52 0.26 0.53 3.66 23.77
 
−
L1014-1 . . . . . . . . . . . . . . . . . . 21221]4955 21 22 08.7 49 55 09 0.42L 0.19 0.69L 8.71
 
−
L973 . . . . . . . . . . . . . . . . . . . . . . 21352]4307 21 35 14.4 43 07 05 1.02 3.56 6.85 13.93
 
−
L1121 . . . . . . . . . . . . . . . . . . . . . 21392]5802 21 39 10.3 58 02 29 0.56 8.87 144.54 424.62
 
−
L1031C . . . . . . . . . . . . . . . . . . . 21446]4704 21 44 35.6 47 04 21 0.25L 0.34L 0.86 13.43
 
−
L1139-2 . . . . . . . . . . . . . . . . . . 21539]5821 21 53 55.2 58 21 25 0.25L 0.25L 5.70 28.84
 
−
L1143 . . . . . . . . . . . . . . . . . . . . . 21570]5842 21 56 58.8 58 42 46 0.51 1.64 4.45 4.74
 
−
L1164 . . . . . . . . . . . . . . . . . . . . . 22052]5848 22 05 09.8 58 48 06 0.25L 5.20 51.52 93.76
 
−
L1221 . . . . . . . . . . . . . . . . . . . . . 22266]6845 22 26 37.2 68 45 52 0.98 3.53 12.36 25.82
 
−
L1251A-1 . . . . . . . . . . . . . . . . 22291]7458 22 29 03.3 74 58 51 0.28L 0.38 0.73 9.12L
 
−
CB 243 . . . . . . . . . . . . . . . . . . . 23229]6320 23 22 52.9 63 20 04 0.26 0.74 2.07 7.94
 
−
0 10 20
 
−
0
 
−
20
 
−
40
 
−
60
 
−
80
 
−
N=348
 
−
All Cores
 
−
0
 
−
20
 
−
40
 
−
60
 
−
80
 
−
N=275
 
−
Starless Cores
 
−
0
 
−
20
 
−
40
 
−
60
 
−
80
 
−
N=72
 
−
Cores with EYSOs
 
−
0 0.5 1 1.5
 
−
0
 
−
20
 
−
40
 
−
60
 
−
N=292
 
−
All Cores
 
−
0
 
−
20
 
−
40
 
−
60
 
−
N=229
 
−
Starless Cores
 
−
0
 
−
20
 
−
40
 
−
60
 
−
N=63
 
−
Cores with EYSOs
 
−
OPTICALLY SELECTED CORES 247
 
−
TABLE 3ÈContinued
 
−
F12km F25km F60km F100km Core Name IRAS or PMSa Name R.A. (1950) Decl. (1950) (Jy) (Jy) (Jy) (Jy)
 
−
L1262A . . . . . . 23238]7401 23 23 48.8 74 01 08 0.25L 0.77 9.64 15.14
 
−
L1271-2 . . . . . . 23585]6653 23 58 30.1 66 53 53 1.54 2.25 40.55L 55.46L
 
−
NOTE.ÈUnits of right ascension are hours, minutes, and seconds, and units of declination are degrees, arcminutes,
 
−
and arcseconds.
 
−
a Names with 1 and 2 added were previously known as class 0 YSOs by Bachiller 1996 and Mardones et al. 1997,
 
−
respectively. Names with 3 and 4 added were identiÐed as PMS by the criteria of Weintraub 1990 and the PMS catalog
 
−
of Herbig & Bell 1988, respectively
 
−
clouds whose distances are known and/or LSR velocities
 
−
[known from a recent CS (2È1) and N (1È0) survey; 2H`
 
−
Lee, Myers, & Tafalla 1999] of our sources are within ^2
 
−
km s~1 of those of the known clouds. Linear sizes of more
 
−
than 80% of all the cores are between 0.05 and 0.35 pc and
 
−
the mean size (^s.e.m.) of the cores is about 0.24 (^0.01) pc.
 
−
Most (about 70%) of the cores with EYSOs have sizes of
 
−
0.15È0.4 pc with a mean of 0.33 (^0.03) pc, while most
 
−
(more than 85%) of starless cores have sizes of 0.05È0.35 pc
 
−
with a mean of 0.21 (^0.01) pc. The sizes of cores with
 
−
EYSOs clearly tend to be larger than those of starless cores.
 
−
Interestingly, this tendency is similar to that of the distribution
 
−
of the sizes of NH cores by BM. We investigated wh3ether this apparent di†erence in core
 
−
sizes originates from any distance e†ect. Figure 6 shows the
 
−
distribution of distances of starless cores and of cores with
 
−
EYSOs, indicating no signiÐcant di†erence in the distances
 
−
between these two groups. Moreover the mean distances
 
−
are nearly same within the range of error, about 227^8 pc
 
−
for starless cores and about 244^19 pc for cores with
 
−
EYSOs. Thus it seems real that the cores with EYSOs are
 
−
usually larger than starless cores by a typical factor of 1.6.
 
−
FIG. 4.ÈDistribution of the apparent angular size of cores. The positions
 
−
of mean angular sizes (mean^s.e.m.) of 3.@7^0@.1, 3.@3^0.@1, and
 
−
5.@1^0.@4 for all cores, starless cores, and cores with EYSOs, respectively,
 
−
are marked with vertical bars in each panel.
 
−
This may mean that larger cores have a greater likelihood
 
−
to form stars since they have more initial mass, or alternatively
 
−
cores with EYSOs may be larger because they have
 
−
been growing for a longer time.
 
−
The aspect ratio (a/b) of cores ranges mostly between 1.5
 
−
and 2.5 for both starless cores and cores with EYSOs (Fig.
 
−
7). The mean (^s.e.m.) aspect ratios are 2.4^0.1, 2.2^0.2,
 
−
and 2.4^0.1 for starless cores, cores with YSOs, and all
 
−
cores, respectively. The most elongated cores are L1271-1
 
−
(10.4) and L698 (10.0). Our measured aspect ratios are
 
−
slightly larger than the value of CB (2.0) for their cores, the
 
−
value of Wood et al. (1994) (1.98) for the IRAS cores, and
 
−
the value of BM (1.9^0.12) for their 41 NH cores. Our measurement for the aspect ratio of cores co3nÐrms that
 
−
most cores are more likely elongated than spherical.
 
−
2.2.3. Spatial Distribution of Selected Cores
 
−
Figure 8 shows the spatial distribution of cores in galactic
 
−
coordinates. This indicates that the cores have been uniformly
 
−
selected from all regions. There seems to be no indication
 
−
that the distribution of cores with EYSOs is di†erent
 
−
from that of starless cores. In this Ðgure we marked Ðve
 
−
distinctive star-forming regions in boxes that contain cores
 
−
FIG. 5.ÈDistribution of the linear size of cores. The positions of mean
 
−
linear sizes (mean^s.e.m.) of 0.24^0.01 pc, 0.22^0.01 pc, and
 
−
0.33^0.02 pc for all cores, starless cores, and cores with EYSOs, respectively,
 
−
are marked with vertical bars in each panel.
 
−
0 200 400 600 800 1000
 
−
0
 
−
50
 
−
100
 
−
150
 
−
200
 
−
N=292
 
−
All Cores
 
−
0
 
−
50
 
−
100
 
−
150
 
−
200
 
−
N=229
 
−
Starless Cores
 
−
0
 
−
50
 
−
100
 
−
150
 
−
200
 
−
N=63
 
−
Cores with EYSOs
 
−
0 2 4 6 8 10 12
 
−
0
 
−
50
 
−
100
 
−
150
 
−
N=308
 
−
Total
 
−
0
 
−
50
 
−
100
 
−
150
 
−
N=249
 
−
Starless Cores
 
−
0
 
−
50
 
−
100
 
−
150
 
−
N=58
 
−
Cores with EYSOs
 
−
248 LEE & MYERS Vol. 123
 
−
FIG. 6.ÈDistance distribution of cores. The distributions of distances
 
−
of starless cores and cores with EYSO are not di†erent. The positions of
 
−
mean distance (mean^s.e.m.) of 231^8 pc, 227^8 pc, and 244^19 pc
 
−
for all cores, starless cores, and cores with EYSOs, respectively, are indicated
 
−
with vertical bars in each panel.
 
−
with similar distances. They are Taurus (Ungerechts &
 
−
Thaddeus 1987), Ophiuchus (de Geus, Bronfman, & Thaddeus
 
−
1990), Lupus (Murphy, Cohen, & May 1986), Chamaeleon
 
−
II, III (Chen et al. 1997), and Vela (Vilas-Boas et al.
 
−
1994). The boundaries of each areas were adopted from the
 
−
references listed above in parentheses.
 
−
2.2.4. Implications of the Ratio of the Number of Cores with EY SOs
 
−
to the Number of Starless Cores
 
−
Our sample gives a ratio [N(cores with EYSOs)]/
 
−
[N(starless cores)] of about 0.31 (B94/306). This ratio is
 
−
important in constraining models of core formation, of
 
−
FIG. 7.ÈDistribution of the aspect ratio for all cores, starless cores, and
 
−
cores with EYSOs. The positions of the mean aspect ratio (mean^s.e.m.)
 
−
of 2.4^0.1, 2.4^0.1, and 2.2^0.2 for all cores, starless cores, and cores
 
−
with EYSOs, respectively, are indicated with vertical bars in each panel.
 
−
which ambipolar di†usion is the best known (Mestel &
 
−
Spitzer 1956). If every core undergoes ambipolar di†usion
 
−
(i.e., dense core formation), infall, and then protostellar
 
−
emission, the value of the ratio [N(cores with EYSOs)]/
 
−
[N(starless cores)] should be approximately [t(life of
 
−
protostar)]/[t(core formation)], assuming that the cores
 
−
have uncorrelated start times. The time t(life of protostar)
 
−
will correspond approximately to the duration of the class
 
−
0]class I stages, based on our IRAS selection criteria
 
−
described in ° 2.1. This time interval has been observationally
 
−
determined to be about (1È5)]105 yr from the
 
−
relative numbers of embedded objects and T Tauri stars
 
−
FIG. 8.ÈDistributions in Galactic coordinates of (a) cores with EYSOs and (b) starless cores listed in Table 2
 
−
No. 1, 1999 OPTICALLY SELECTED CORES 249
 
−
(Myers et al. 1987; Wilking, Lada, & Young 1989; Kenyon
 
−
et al. 1990). The time t(core formation) should be the time
 
−
that the core is detectable at its typical observed density,
 
−
according to its formation model. The cores in our catalog
 
−
(most of which have been selected from Lynds classes 5 and
 
−
6) are thought to have visual extinctions of 4.5È6 mag in
 
−
their centers (Cernicharo & Bachiller 1984). This means that
 
−
the mean number density in the center of our optically
 
−
selected cores is about (6È8)]103 cm~3, assuming a core
 
−
diameter of 0.24 pc from our statistics and the relationship
 
−
N(H cm~2 from Dickman (1978) where 2)B1]1021Av
 
−
N(H and are column density of and magnitude of 2) Av Hvisual extinction, respectively. Therefor2e the time that the
 
−
core has gas density (6È8)]103 cm~3 can be obtained from
 
−
ambipolar di†usion models. We Ðnd that di†erent models
 
−
give slightly di†erent time periods for gas to have such
 
−
density. The most detailed model ““B of Ciolek & Mous- UV ÏÏ
 
−
chovias (1995) gives about (5.5È6.7)]106 yr, the model by
 
−
Li (1998) about (3.5È4.1)]106 yr, and the model by Palla
 
−
& Galli (1997) about (8.7È13.4)]106 yr for a core with a
 
−
size of 0.24 pc and magnetic Ðeld strength of 30 kG. Thus
 
−
present ambipolar di†usion models seem to indicate that
 
−
detectable cores in our sample will be condensed within
 
−
about (3.5È13.4)]106 yr, after which the cores will
 
−
undergo dynamical, star-forming collapse. Thereby, the predicted
 
−
ratios of [t(life of protostar)]/[t(core formation)] is
 
−
[(1È5)]105]/[(3.5È13.4)]106]B0.007È0.14, which is
 
−
smaller than our empirical value (0.31) by a factor of about
 
−
2È44. This discrepancy between model predictions and our
 
−
data is also seen for the Ðve star forming regions ; the
 
−
empirical ratios are 0.39 (B4/36) for Taurus, 0.46 (B9/41)
 
−
for Ophiuchus, 0.33 (B9/27) for Lupus, 0.23 (B3/13) for
 
−
Chamaeleon II and III, and 0.38 (B5/13) for Vela.
 
−
As a result, the timescale of ambipolar di†usion for core
 
−
formation in the present models seems to be too long, suggesting
 
−
that the models of ambipolar di†usion need to be
 
−
modiÐed or perhaps that faster mechanisms of core formation
 
−
should be also considered (cf. Tafalla et al. 1998). We
 
−
suggest that the typical lifetime of starless cores [Z(6È8)
 
−
]103 cm~3] may be about 3 times longer than the duration
 
−
of the class 0 and class I phases, i.e., about (0.3È
 
−
1.6]106) yr, which is shorter than the ambipolar model
 
−
prediction by a factor of 2È44. A similar conclusion was
 
−
reached by Jijina, Myers, & Adams (1998) based on statistics
 
−
of NH cores with and without associated stars. 3
 
−
3. CONCLUSION
 
−
In this paper we present a new catalog of 406 dense cores
 
−
optically selected by using the STScI Digitized Sky Survey
 
−
(DSS). We have imaged areas of 0.52 or 1.0 deg2 around
 
−
already known numerous NH and C18O cores, every Lynds class 5 and 6 cloud (Lynds3 1962), and every southern
 
−
Hartley et al. (1986) class A cloud, to identify every local
 
−
minimum of intensity in each Ðeld and to select the darkest
 
−
and best resolved minima. For the identiÐed 406 sources, we
 
−
used the IRAS Point Source Catalog to determine which
 
−
have associated point sources and used the criteria for PMS
 
−
stars by Weintraub (1990) and the catalog of PMS stars by
 
−
Herbig & Bell (1988) to Ðnd possible PMS stars associated
 
−
with the cores. From these surveys, 306 starless cores with
 
−
neither an embedded YSO (EYSO) nor a preÈmainsequence
 
−
(PMS) star, 94 cores with EYSOs (one core has
 
−
both an EYSO and a PMS star), and six cores with only a
 
−
PMS star are found. This list of dense cores will be a useful
 
−
database for an extensive systematic study of dense cores for
 
−
a better understanding of the early stages of star formation.
 
−
Our fairly complete sample of most opaque cores gives
 
−
representative statistics of physical parameters of dense
 
−
cores. Most cores are found to have an apparent angular
 
−
size of 1@È4@ and a linear size of D0.1È0.3 pc, with an
 
−
average of 0.24 pc. Interestingly, the sizes (mean:
 
−
0.33^0.03 pc) of the cores with EYSOs are usually larger
 
−
than those (mean: 0.21^0.01 pc) of the starless cores. The
 
−
mean aspect ratio of cores is 2.4^0.1, conÐrming that most
 
−
cores are more likely elongated than spherical.
 
−
The ratio of [N(cores with EYSOs)]/[N(starless cores)]
 
−
for our sample is about 0.31 (B94/306). This value is much
 
−
higher than expected from the relative time scales
 
−
([t(life of protostar)]/[t(core formation)]B[(1È5)]105]/
 
−
[(3.5È13.4)]106]B0.007È0.14) of ambipolar di†usion of a
 
−
core [with gas densityZ(6È8)]103 cm~3] and the life of a
 
−
protostar. The statistics of our sample indicate that the
 
−
ambipolar di†usion timescale predicted by present models
 
−
for dense core formation may be too long. The typical lifetime
 
−
of starless cores is suggested to be about 3 times longer
 
−
than the duration of the class 0 and class I phases, i.e., about
 
−
(0.3È1.6)]106 yr, which is shorter than the ambipolar
 
−
model predictions by a factor of 2È44.
 
−
C. W. L acknowledges the Ðnancial support from the
 
−
1996 Overseas Postdoctoral Support Program of Korea
 
−
Research Foundation. C. W. L also thanks the Harvard-
 
−
Smithsonian Center for Astrophysics for support while
 
−
working on this project. We would like to thank Lori Allen
 
−
and August Muench for their careful reading of our manuscript
 
−
and an anonymous referee for his useful comments.
 
−
This research was supported by NASA Origins of Solar
 
−
System Program, grant NAGW-3401.
 
−
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Murphy, D. C. 1985, Ph.D. thesis, Massachusetts Inst. of Technology
 
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Murphy, D. C., Cohen, R., & May, J. 1986, A&A, 167, 234
 
−
Myers, P. C., Fuller, G. A., Mathieu, R. D., Beichman, C. A., Benson, P. J.,
 
−
Schild, R. E., & Emerson, J. P. 1987, ApJ, 319, 340
 
−
Myers, P. C., Linke, R., & Benson, P. J. 1983, ApJ, 264, 517 (MLB)
 
−
Neckel, T., & Klare, G. 1980, A&AS, 42, 251
 
−
Onishi, T., Mizuno, A., Kawamura, A., Ogawa, H., & Fukui, Y. 1996, ApJ,
 
−
465, 815
 
−
Palla, F., & Galli, D. 1997, ApJ, 476, 38
 
−
Postman, M. 1996, in Distribution of the Astronomy Community of the
 
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Compressed Digitized Sky Survey (Baltimore: Space Telescope Science
 
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Inst.)
 
−
Rogers, A. W. 1960, MNRAS, 120, 163
 
−
Schmidt, E. G. 1975, MNRAS, 172, 401
 
−
Schwartz, R. D. 1991, in Low Mass Star Formation in Southern Molecular
 
−
Clouds, ed. B. Reipurth (ESO Sci. Rep. 11) (Garching: ESO), 93
 
−
Shu, F. H., Adams, F. C., & Lizano, S. 1987, ARA&A, 25, 23
 
−
Snell, R. L. 1981, ApJS, 45,121
 
−
Straizys, V., Cernis, K., Kazlauskas, A., & Meistas, E. 1992, Baltic Astron.,
 
−
1, 149
 
−
Tafalla, M., Mardones, D., Myers, P. C., Caselli, P., Bachiller, R., &
 
−
Benson, P. J. 1998, ApJ, 504, 900
 
−
Tody, D. 1993, in ASP Conf. Ser. 52, Astronomical Data Analysis Software
 
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and Systems II, ed. R. J. Hanisch, R. J. V. Brissenden, & J. Barnes (San
 
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Francisco: ASP), 173
 
−
Tomita, Y., Saito, T., & Ohtani, H. 1979, PASJ, 31, 407
 
−
Ungerechts, H., & Thaddeus, P. 1987, ApJS, 63, 645
 
−
VanHilst, M. 1990, BAAS, 22, 935
 
−
Vilas-Boas, J.W. S., Myers, P. C., & Fuller, G. A. 1994, ApJ, 433, 96
 
−
Viotti, N. R. 1969, Mem. Soc. Astron. Italiana, 40, 75
 
−
Weintraub, D. A. 1990, ApJS, 74, 575
 
−
Wilking, B. A., Lada, C. J., & Young, E. T. 1989, ApJ, 340, 823
 
−
Wood, D. O. S., Myers, P. C., & Daugherty, D. A. 1994, ApJS, 95, 457
 
  
−
This didn't format well.  Please let me know if there is a better way to send papers
+
--[[User:Mcdonald|Mcdonald]] 15:47, 15 January 2008 (PST)   Here is John's colored image made in Austin again 15 x 15 arcmin:
−
Thanks
+
  [[Image:LDN880 by John.jpg]]
−
--[[User:Guastella|Guastella]] 20:48, 8 January 2008 (PST)
 
−
Pete
 
  
 
=LDN 1340=
 
=LDN 1340=
 +
 +
[[image:ldn1340possred.gif|left]]  LDN 1340 in POSS-red.  image is 0.25 deg on a side. --[[User:Rebull|Rebull]] 14:09, 14 January 2008 (PST)
 +
  
 
--[[User:Rebull|Rebull]] 20:14, 8 January 2008 (PST)  Here's a summary of the latest developments on this object:
 
--[[User:Rebull|Rebull]] 20:14, 8 January 2008 (PST)  Here's a summary of the latest developments on this object:
 +
  
 
One of you (Peter?) suggested this object - and it was a fabulous suggestion.  Beautiful in the optical, with IRAS sources, a handful of existing literature, and no Spitzer. Perfect!  The icing on the cake was that it's visible in the Spring.
 
One of you (Peter?) suggested this object - and it was a fabulous suggestion.  Beautiful in the optical, with IRAS sources, a handful of existing literature, and no Spitzer. Perfect!  The icing on the cake was that it's visible in the Spring.
Line 1,439: Line 81:
 
[END]
 
[END]
  
 +
 +
--[[User:Guastella|Guastella]] 20:48, 8 January 2008 (PST)
 
In case we are still looking at this here is the 2005 Abstract
 
In case we are still looking at this here is the 2005 Abstract
−
Submillimetre Observations of an Intermediate-Mass Star Forming Cloud Core J. O’Linger1, G. H. Moriarty-
+
Submillimetre Observations of an Intermediate-Mass Star Forming Cloud Core J. O’Linger, G. H. Moriarty-
−
Schieven2, and G. A. Wolf-Chase3,4, 1Spitzer Science Center (joanno@ipac.caltech.edu), 2National Research Council
+
Schieven, and G. A. Wolf-Chase
−
of Canada, JAC (g.schieven@jach.hawaii.edu), 3Adler Planetarium & Astron. Mus. (gwolfchase@
+
 
−
adlerplanetarium.org), 4Univ. of Chicago (grace@horta.uchicago.edu).
+
[http://adsabs.harvard.edu/abs/2005AAS...20718413O ADS link to AAS abstract]
−
We present preliminary results in an ongoing, comprehensive
+
 
−
investigation of the star formation activity
+
[http://adsabs.harvard.edu/abs/2005prpl.conf.8600O ADS link to PPV abstract]
−
in LDN 1340. This dark nebula (opacity class 5) is
+
 
−
located approximately 600 pc away, in the constellation
+
--[[User:Rebull|Rebull]] 09:37, 9 January 2008 (PST) I talked to JoAnn again today, and she thinks that maybe doing just a piece of the cloud would be a good idea. She showed me some of her supporting data, and indeed this is a really cool area. We could do just a part of it now, and eventually, she'll map the rest of the cloud as well.
−
Cassiopeia. Due to various reflection nebulae and
+
 
−
a significant number of embedded IRAS sources, it was
+
Here's her poster from today: [[Media:joann2008poster.pdf]]
−
identified as a region of active star formation by Kun
+
 
−
et al., 1994 [1].
+
[END]
−
Star formation occurs when the parent molecular
+
--[[User:Mcdonald|Mcdonald]] 15:51, 15 January 2008 (PST)  15 x 15 colored image:
−
cloud collapses to form young stars of different
+
  [[Image:ldn1340.jpg]]
−
masses. A number of investigators have studied various
+
 
−
mechanisms, which might trigger and/or accelerate
+
=LDN 951=
−
this collapse and fragmentation process [2]. Clearly,
+
 
−
the ionization fronts and stellar winds associated with
+
From:  cdewolf@chsd.us
−
massive stars have a significant impact on their natal
+
How does LDN 951 look? Assuming I did my query right, it also hasn't been looked at by Spitzer. I found it on a list of LDNs that have visual opacities of 6 in a paper by Visser et. al, 2002. There's another, but it doesn't look as interesting.
−
environments, as do the shock waves from the supernovae
+
Cris L. DeWolf
−
at the ends of their brief lifetimes. These effects
+
[[image:LDN951.red.jpg]]
−
may induce subsequent generations of star formation,
+
 
−
but if the turbulence created within the ambient cloud
+
 
−
is sufficiently disruptive, it may actually disperse the
+
--[[User:Rebull|Rebull]] 14:00, 9 January 2008 (PST) ooh, this is a nice one!  you're right, it doesn't have any Spitzer observations yet.  This might very well be a good candidate!  [END]
−
cloud, causing star formation to cease [3]. To date,
+
 
−
studies of triggered star formation have tended to concentrate
+
--[[User:Dewolf|Dewolf]] 06:00, 12 January 2008 (PST)There was a study of IRAS associations with dark clouds (Parker, N.D., 1988) that appears to indicate a good chance of there being a YSO in LDN 951. Here's a link to the article.
−
on the most massive of stars (i.e., O and early
+
[http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988MNRAS.235..139P&db_key=AST&link_type=ABSTRACT&high=4788c3397d22375]
−
B-types) and the star-forming regions in their immediate
+
[END]
−
vicinities; the question of whether or not intermediate-
+
 
−
mass stars (such as late B and early A-types) are
+
--[[User:Mcdonald|Mcdonald]] 15:54, 15 January 2008 (PST)  A 15 x 15 arcmin colored image:
−
capable of causing similar triggering events has not
+
  [[Image:ldn951.jpg]]
−
been thoroughly examined.
+
 
−
Submillimeter maps, at 450 and 850 microns, of a
+
=Other targets=
−
portion of the L1340 cloud (L1340B) were obtained
+
 
−
with the SCUBA bolometer array on the James Clerk
+
--[[User:Rebull|Rebull]] 11:42, 9 January 2008 (PST) I found two posters today on Lynds clouds - L1221 and L988e.  L1221 has Spitzer data which is pretty cool; L988 doesn't have any Spitzer data. Take a look at the other bands and references and see if it would be interesting....
−
Maxwell Telescope located on Mauna Kea, Hawaii.
+
[END]
−
The image is presented in Figure 1. We have observed
+
 
−
more than two dozen submillimeter sources in a ~17’
+
--[[User:Rebull|Rebull]] 14:09, 14 January 2008 (PST) nevermind; the L988 image is pretty much just a star field. [END]
−
by 12’ region, most of them undetected at any other
+
 
−
wavelength. A few of them are associated with previously
+
[[image:l1014.jpg|left]]
−
identified IRAS or 2MASS sources. We have
+
--[[User:Rebull|Rebull]] 14:27, 14 January 2008 (PST) just for comparison, here is a spitzer composite image of L1014. we'd be very lucky to find something like this, but this is the hope. [END]
−
also mapped the region in the emission from the J=3-2
+
 
−
transition of CO.
+
--[[User:Rebull|Rebull]] 13:44, 14 January 2008 (PST) David added some general target selection stuff to the [https://coolwiki.ipac.caltech.edu/index.php/Talk:Lynds_Target_Selection talk page] [END]
−
As can be seen in Figure 1, most of our detected
+
 
−
sub-mm sources are located in ridges, like “pearls in a
+
 
−
string”, which surround voids. Also shown in this
+
--[[User:Rebull|Rebull]] 10:48, 15 January 2008 (PST) Out of David's top 16 suggestions, the only ones wihtout existing spitzer data are ldn 
−
figure are known low- and intermediate-mass stars.
+
1357 (right on the edge of some existing spitzer data) and ldn 1358. you must be doing something right, as you're hitting popular objects. ;)   [END]
−
Morphology and classifications of these objects suggest
+
 
−
that we are witnessing triggered star formation.
+
--[[User:Rebull|Rebull]] 14:19, 21 January 2008 (PST) but really from jan 20: tim sent this in email:
−
For example, we discuss the case of the Herbig Be star
+
  I have been doing some looking at the Lynds targets.  I'm attaching pics of LDN 1598 and LDN 1340.
−
known as “R3” in the paper by Kun et al. [1].
+
  I could not find anything in ADS about either of these targets, so it looks like they have not been
−
In Figure 1, the sources closest to R3 are T Tauri
+
  studied a great deal. I like the fact that you have a dark area next to a fairly rich star field
−
stars (class II) candidates (determined from 2MASS
+
  (especially with 1598). This would tend to indicate a dense nebulous area. the images are 5'x5'. (targets suggested by Tim Spuck)
−
database using the classification scheme of Lee et al.
+
here's the graphics: (L1598 first, then L1340):
−
[3], while beyond those objects lies a ridge containing
+
[[image:tim_l1598.jpg]] [[image:tim_l1340.jpg]]
−
only submillimeter sources and Class I candidates.
+
 
−
Assuming that the ridge represents the location of the
+
--[[User:Rebull|Rebull]] 14:26, 21 January 2008 (PST) actually, i get 19 references for ldn 1598, and 15 for L1340, both using simbad... [END]
−
ionization front from R3, calculations to estimate the
+
 
−
timescale involved (using as the propagation velocity
+
--[[User:Spuck|Spuck]] 05:37, 22 January 2008 (PST)  Luisa, just for future reference, I thought ADS was a more complete database for identification of current research. I assume this is not the case since you found many references in simbad. Is that correct?  Thanks, Tim  [END]
−
the sound speed from Lee et al. [3], i.e. 10 km/s), show
+
 
−
that the time it would take for the ionization front to
+
--[[User:Spuck|Spuck]] 06:57, 22 January 2008 (PST)  Ok ... I think I may have answered part of my question.  I was seaching on LDN1598 and coming up with nothing, but if I search on L1598 or L1340 I am at least coming up with something in ADS (one for 1598, and seven for L1340).  I need to play with the parameters a bit. [END]
−
reach the five nearest T Tauri candidates would be of
+
 
−
order 2.3Ma (TT3) to ~11Ma (TT1).
+
--[[User:Rebull|Rebull]] 17:57, 22 January 2008 (PST) they're different sorts of databases, with different strengths and weaknesses.  ADS is driven by the literature itself, whereas SIMBAD is driven more by object lists.  ADS is usually more complete.  But, for example, some of the references for L1685 don't actually call it L1685 anywhere in the paper.  ADS may or may not have the information that those papers really do have data about that object - sometimes ADS knows, and sometimes ADS doesn't.  Someone at the SIMBAD end did realize (or at least THINKS) that the objects are the same, and has (hopefully correctly) tied the object to the paper.  SIMBAD often requires a human to make the association between synonyms for certain objects, and this can be fallible, especially for the more obscure objects.  ADS is generally more accurate in the following sense - SIMBAD may quote a spectral type, but to be sure that whatever object you are looking at really has that type, track down the original papers and make sure that the actual original paper really does cite that type.  More obscure papers are rarely in SIMBAD, but they can be found in ADS.  ADS and SIMBAD are heavily interlinked, so there's a lot of ways to get between them. [END]
−
In this poster, we will discuss the evidence for triggered
+
 
−
star formation within this cloud, based on dust
+
--[[User:Dewolf|Dewolf]] 22 Jan 2008 10:19:06 (question submitted via regular email): I'd seen some images [before] with the large pixel areas as well. How do you find a potential IRAS source in a small LDN with such poor resolution? [END]
−
continuum, CO, 2MASS and other data.
+
 
−
References:
+
--[[User:Rebull|Rebull]] 10:19, 22 January 2008 (PST):
−
1. Kun, M., et al. 1994, A&A, 292, 249
+
Your question really has a two-part answer.
−
2. Elmegreen, B. 1998, Observations and Theory
+
 
−
of Dynamical Triggers for Star Formation, ed. C.E.
+
The first part is that I'm not detecting sources by eye.  I'm relying upon the computer-generated IRAS Point Source Catalog (PSC) and Faint Source Catalog (FSC) which are described along with the rest of the IRAS mission
−
Woodward, J.M. Shull, & H.A. Thronson, ORIGINS,
+
information here: http://irsa.ipac.caltech.edu/IRASdocs/iras.html
−
ASP Conference Series 148
+
 
−
3. Lee, H., Chen, W., Zhang, Z., & Hu, J. 2005,
+
If you get into the documentation, you will find that the catalog consists of, among other things, measurements at each of the 4 IRAS wavelengths, and a quality flag for each of the 4 bands.  This quality flag is REALLY
−
Triggered Star Formation in the Orion Bright-Rimmed
+
IMPORTANT, as it tells us whether the computer thought it was a real detection at each band, or just an upper limit at a particular band. Because the resolution of IRAS is so poor, indeed, it can be fooled.
−
Clouds, arXiv:astro-ph/0502061 v1
+
 
−
Protostars and Planets V 2005 8600.pdf
+
One of the objects in our shortlist below really did have a recognizable clear point source right on the center of the object at 25 um. But, the rest, I agree, I'd be hard-pressed to identify the source by eye. That doesn't mean it's not there, however.  The computer is really good at finding real, faint sources.  When we go to write this up, we really should pay attention to whether the computer felt it was a point source just at 100 um and not at 12 or 25 um.  For this subset of objects, I am cheating a little because several of them have observations at other wavelengths, enough so that I know there's a real source there, so I didn't go check the quality flags for those objects.
−
Figure 1: 850 μm image of theL1340B intermediate-mass star forming region. The field shown is approximately
+
 
−
17’x11’ in extent. Known A and B stars are indicated (see legend above), as well as candidate T Tauri stars
+
The second aspect of the answer is that when we go look with Spitzer, it could very well be that the source dissolves away into background nebulosity, or breaks into pieces.  We have an image at 24 um of something in the Perseus star-forming region that appears in the IRAS catalog as a single object, IRAS 03388+3139.  But, when we look with Spitzer, it breaks up into 9 objects.  This stuff appeared in Rebull et al., 2007, ApJS, 171, 447 (also findable in astro-ph, look near Jan 2007), along with an analysis of what IRAS sources dissolved away completely into nebulosity when viewed with Spitzer.  The nebulosity is very complex here, so it happens.
−
and previously unidentified scuba sources.
+
[END]
−
Protostars and Planets V 2005 8600.pdf
+
 
 +
=A (The?) Shortlist=
 +
 
 +
Goal: find anywhere from one to a few LDN likely to host young stars so that we not only have a pretty picture but also find some new baby stars.  If we are going to ask for more than one cloud, they need to have different properties, so that we can explain that we are looking at THIS sort and THAT sort to compare.  And we can (should) also say we will mine the Spitzer archive for more examples.
 +
 
 +
==Luisa's Favorites==
 +
 
 +
{| border="1"
 +
|LDN
 +
|Image
 +
|Notes
 +
|-
 +
|951
 +
|[[image:ldn951_possred.jpg]] (POSS/Red, 0.25 deg on side)
 +
|
 +
* from cris (see above.)
 +
* opacity class 6 (good, deep and dark)
 +
* 'linear' (as opposed to 'blobby')
 +
* (Visser et al. 2002, AJ, 124, 2756) part of the cygnus rift, 700 pc away, max extinction Av=10, just 4.7 Msun in cloud
 +
* IRAS source 21186+4320
 +
* (ref?) two submm 'starless cores' here : in 1950 coordinates 21:18:20 +43:19:17 and 21:18:22.9 +43:19:51 -> we might not find anything, but we might find some of the youngest stars forming here.
 +
* visible to spitzer through tomorrow 1/22 (argh!); next window june 27-sep 10.
 +
*IRAC total time 907 sec, MIPS total time 3313 seconds.  IRAC: [[media:ldn951_withirac.gif]] (irac has two fields of view, portrayed by the two colors; the region covered by both colors is the region we'll get with all 4 irac bands [3.6, 4.5, 5.8, and 8 um].  note that the specific portion of sky that we will cover rotates, so these observations are designed to catch as much of the LDN as i can and still be independent of rotation angle.)  MIPS: [[media:ldn951_withmips.gif]] (MIPS has 3 cameras, but we're only using 2 -- indicated by the two colors, 24 and 70 um. 
 +
* with irac we will see mostly stars, some nebulosity.  we need at least MIPS-24, which is 1191 seconds of the 3313 seconds; mips 24 will help us find stars, but also find the nebulosity.  in this specific case, where we have some submm cores, mips70 is important too, as it might be just at mips70 that we see these submm cores.  note that i get a little too much sky at 24 and not quite enough at 70; i'm constrained by the choices i have in the AOR construction, and i'm optimizing for science and time, not necessarily a pretty picture.
 +
*TOTAL TIME: 1.2 hrs. (4 IRAC plus 2 MIPS)
 +
|-
 +
|425
 +
|[[image:ldn425_possred.gif]] (POSS/Red, 0.25 deg on side)
 +
[[image:ldn425_mycenter_possred.gif]]
 +
|
 +
* from cris' ppt based on some subset of my target weeding.
 +
* opacity class 5 (good, pretty deep and dark)
 +
* 'blobby' (as opposed to 'linear')
 +
* Lee and Myers (1999, ApJS, 123, 233) find a YSO here (1950 coords: 17 44 15.4 −04 34 07)
 +
* IRAS source 17442−0433
 +
* Connelley et al (2007 AJ 133, 1528) find a new NIR reflection nebula here, suggestive that a YSO is illuminating the nebula, and that we will see something pretty at IRAC bands.
 +
* the part that is the center of the coordinates given by lynds (center of image at left) seems offset from the darkest part as seen in POSS. X's in graphic at left are the IRAS point sources in this region; the northernmost one is the one listed in the literature. there is not much to the dark cloud north of the image region shown at left.  I'm taking as the center 17:46:55 -04:36:25; see second graphic at left.
 +
* visible to spitzer apr 12-may 23, then sep 21-nov 2.
 +
* IRAC total time 657 seconds ([[media:ldn425_mycenter_possred_withirac.gif]]) MIPS-24 total time only 395 seconds. Harder to justify 70 um time too here, since it will be expensive and it's not entirely clear what we will see. Could simply plan to jump on the data right away and ask for more time to do 70 if it seems likely to be interesting. ([[media:ldn425_mycenter_possred_withmips.gif]] - box is "my center" for this observation and x's are IRAS sources.)
 +
*TOTAL TIME: 0.3 hrs. (4 IRAC plus 1 MIPS)
 +
|-
 +
|981
 +
|[[image:ldn981_possred.gif]] (POSS/Red, 0.3 (not 0.25!) deg on side)
 +
|
 +
* from cris' ppt based on some subset of my target weeding.
 +
* opacity class 6 (good, deep and dark)
 +
* 'linear' (as opposed to 'blobby')
 +
* Quanz et al. (2007, ApJ, 656, 287, also astro-ph/0610786 -- see http://arxiv.org/abs/astro-ph/0610786 for free copy of paper) has a very interesting article about the structures around V1331 Cyg, a known YSO.  They were studying the immediate environment of this thing using HST, but it is at the end of one of the filaments associated with LDN 981.  One of the questions they address in this paper is whether or not V1331 Cyg formed on its own, or with 'friends.'  They talk in their paper (see sections 4.2 and 4.3) about whether some objects found in the LDN black parts are real YSOs or not, and they conclude based on available evidence that they are not YSOs.  BUT, maybe they just weren't looking in long enough wavelengths.  We might find that these stars really are YSOs... or we may not.  We may confirm that yes, they are just foreground objects superimposed on the dark lanes of the nebula.  V1331 Cyg is just on the edge of the image, to the upper left, at the end of that dark lane, with the funny circular bright nebula (that was what Quanz et al studied with HST).
 +
*[[media:timldn981.jpg| image from tim comparing more wavelengths]]
 +
*[[media:crisldn981.jpg| image from cris comparing scales]]
 +
* visible to Spitzer through jan 27 (argh!), then june 26-feb 3 (not a typo, nice and long!)
 +
* some existing MIPS data to the east (left) and north (up) which we could grab and add in to our maps.
 +
* IRAC total time 2152 sec ([[media:ldn981_possred_withirac.gif]]) **need to add a constraint to both IRAC and MIPS that it be done before sep 15 (1 for MIPS) in order to cover the region we want. (usually constraints are bad, but i'd have to ask for more time otherwise, and we are giving them a large window, so it should be ok.) MIPS 24 only 1191 sec. ([[media:ldn981_possred_withmips24.gif]]) Again, somewhat hard to justify asking for 70 um time, but this time, V1331 Cyg is an IRAS source, so ''maybe'' worth it. MIPS-70 alone is another 6079 sec. (!) ([[media:ldn981_possred_withmips70.gif]])
 +
*TOTAL TIME: 0.9 hrs (4 irac plus 1 mips) or 2.6 hrs (4 irac plus 2 mips)
 +
|-
 +
|1143
 +
|[[image:ldn1143_possred.gif]] (POSS/Red, 0.3 deg on side - now spot won't let me do 0.25, ??)
 +
|
 +
* from cris' ppt based on some subset of my target weeding.
 +
* opacity class 6 (good, deep and dark)
 +
* 'blobby' (as opposed to 'linear')
 +
* Lee and Myers (1999, ApJS, 123, 233) find a YSO here (1950 coords: 21 57 03.0 58 42 25)
 +
* IRAS source 21569+5842
 +
* Connelley et al. (2007 AJ 133, 1528) find a new NIR reflection nebula here, suggestive that a YSO is illuminating the nebula, and that we will see something pretty at IRAC bands.
 +
* Magnier et al. (1999, A&A, 352, 228) find something they call a "transition object" here, and is noted specifically as a "very red star." It's likely we will be better able to tell what this thing is.
 +
* visible to Spitzer through feb 22 (too soon to schedule us) and then jul 23-mar 2 (again, not a typo, nice and long).
 +
* IRAC total time 907 sec ([[media:ldn1143_possred_withirac.gif]] - box is 'target', x's are iras sources), MIPS-24 total time 1191 sec (just mips24, not mips70 too, again hard to justify) ([[media:ldn1143_possred_withmips24.gif]]).
 +
* TOTAL TIME: 0.6 hrs (4 irac plus 1 mips)
 +
|-
 +
|1598
 +
|[[image:ldn1598_possred.gif]] (POSS/Red, 0.3 deg on side - now spot won't let me do 0.25, ??) x's are IRAS sources
 +
|
 +
* from Tim based on some subset of my target weeding
 +
* opacity class 5 (good, pretty deep and dark)
 +
* 'blobby' (as opposed to 'linear')
 +
* 19 refs in SIMBAD. 
 +
* IRAS 05496+0812, also WB89 718, also HH 117 VLA 1 (so clearly several people have looked here before).  This is part of the lambda Ori complex, apparently, and maybe related to alpha Ori (Betelgeuse).  There is a lot of Spitzer data covering parts of the lambda Ori complex, but evidently not this cloud and its friend, L1599.  I will ask my friends who are studying the lambda Ori complex about this object.
 +
* Wu et al. (2004, A&A, 426, 503) studied outflows and claim to find one here, placing the cloud at 0.9 kpc.  Another paper, Hilton & Lahulla (1995, A&AS, 113, 325) cite Schwartz et al (1988) also at 900 pc.
 +
* Rodriguez & Reipurth (1998) find the exciting source for HH117 here; our observations as planned will also cover the HH object itself.
 +
* visible to spitzer mar 21-apr 29, then oct 18-nov 28.
 +
* IRAC total time 907 sec ([[media:ldn1598_possred_withirac.gif]] - box is 'target', x's are iras sources), MIPS-24 total time 1191 sec (just mips24, not mips70 too, again hard to justify) ([[media:ldn1598_possred_withmips24.gif]]).
 +
* TOTAL TIME: 0.6 hrs (4 irac plus 1 mips)
 +
|-
 +
|1685
 +
|[[image:ldn1685_possred.gif]] (POSS/Red, 0.25 deg on side)
 +
|
 +
* from Chelen based on some subset of my target weeding
 +
* opacity class 5 (good, pretty deep and dark)
 +
* 'blobby' (as opposed to 'linear')
 +
* 10 references in SIMBAD; aliases include BHR 157, [CB88] 73, Barnard 56, DCld 352.9+04.8
 +
* Huard et al. (1999, ApJ, 526, 833) does NOT detect this in the submm, and is able to constrain the distance at <160 pc (in front of the ophiuchus clouds).
 +
* I think it was also undetected by Bourke et al. (1995 MNRAS) in ammonia.
 +
* there is an IRAS source here; see x's in figure to left. IRAS 17056-3204 is the one closest to the center.
 +
* visible to spitzer apr 4-may 13 then sep 14-oct 24
 +
* IRAC total time 907 sec ([[media:ldn1685_possred_withirac.gif]] - box is 'target', x's are iras sources), MIPS-24 total time 1191 sec (just mips24, not mips70 too, again hard to justify) ([[media:ldn1685_possred_withmips24.gif]]).
 +
* TOTAL TIME: 0.6 hrs (4 irac plus 1 mips)
 +
|}
 +
 
 +
the AOR file to load into spot is here: [[media:lyndsaors.aor.txt]] - i had to add a ".txt" extension to get the wiki to accept it, but you should save the file to disk and rename it as just ".aor" and then Spot will recognize it as an AOR file.
 +
 
 +
==Middle-of-the-road candidates==
 +
Usually they're just here because there's no good reason to reject them, but others seem prettier or more likely to host stars.
 +
*LDN 470 - small, opacity class=6. 
 +
*LDN 1225 - bigger, opacity class 4 only (too thin?)
 +
*LDN 1125 - opacity class=5, blotchy/blobby, same as Barnard 152, Lee and Myers say YSO but appears in 'starless core' papers.
 +
*LDN 1139 - opacity class=5, blotchy/blobby, Lee and Myers say YSO but appears in 'starless core' papers.
 +
 
 +
==Rejects, and reasons:==
 +
*LDN 880 - lee and myers say no YSO; rather thin in optical images, and might just see through it in spitzer.
 +
*LDN 769 - lee and myers say no YSO; mentioned in several other "starless core" papers.
 +
*LDN 778 - many simbad refs (>40!) but most of them are 'starless core' papers
 +
*LDN 1041 - image looks like a plain star field
 +
*LDN 1082 - image looks like a plain star field
 +
*LDN 1340 - nice image, but consensus from the group was that they wanted to work in a 'new' region.
 +
 
 +
=Voting and Ranking=
 +
 
 +
If the editing of the table in the wiki intimidates you, or you're worried about making sure your vote appears under your column (this can be tricky), feel free to just email me your ranking, and I'll enter it here.  "1" is high (most favorite), "6" is low (least favorite).  So as not to bias you, I won't put in my votes until the very end.
 +
 
 +
{| border="1"
 +
|LDN
 +
|Pete
 +
|Chelen
 +
|David
 +
|John
 +
|Cris
 +
|Tim
 +
|Luisa
 +
|AVERAGE
 +
|-
 +
|951
 +
|6
 +
|5
 +
|1
 +
|4
 +
|5
 +
|5
 +
|5
 +
|'''4.4'''
 +
|-
 +
|425
 +
|2
 +
|2
 +
|
 +
|2
 +
|2
 +
|2
 +
|3
 +
|'''2.2'''
 +
|-
 +
|981
 +
|1
 +
|1
 +
|2
 +
|1
 +
|1
 +
|1
 +
|1
 +
|'''1.1'''
 +
|-
 +
|1143
 +
|3
 +
|4
 +
|3
 +
|5
 +
|3
 +
|4
 +
|2
 +
|'''3.4'''
 +
|-
 +
|1598
 +
|4
 +
|6
 +
|
 +
|3
 +
|4
 +
|3
 +
|4
 +
|'''4.0'''
 +
|-
 +
|1685
 +
|5
 +
|3
 +
|
 +
|6
 +
|6
 +
|6
 +
|6
 +
|'''5.3'''
 +
|}
 +
 
 +
Rank-ordered list is therefore:
 +
*LDN 981 (rank 1.1) - 0.9 hrs spitzer time
 +
*LDN 425 (rank 2.2) - 0.3 hrs spitzer time
 +
*LDN 1143 (rank 3.4) - 0.6 hrs spitzer time
 +
*LDN 1598 (rank 4.0) - 0.6 hrs spitzer time
 +
*LDN 951 (rank 4.4) - 1.2 hrs spitzer time
 +
*LDN 1685 (rank 5.3) - 0.6 hrs spitzer time
 +
 
 +
I would counsel that you write a proposal for the top two clouds.  They have some different properties, and the total time request of 1.2 hrs is not completely outrageous.
 +
 
 +
--[[User:Dewolf|Dewolf]] 08:54, 29 January 2008 (PST)The paper that Luisa referred to in her discussion of LDN 981 is worth a read as we prepare our proposal. Here is a direct link to a pdf of it [[media:0610786v1.pdf]]. The authors suggest that V1331 Cyg evolved from one of the filaments in this linear cloud. To me, this implies a strong possibility of additional YSOs in the cloud. What do you think? [END]
 +
 
 +
--[[User:Rebull|Rebull]] 13:02, 30 January 2008 (PST) Yep, i think it's a strong possibility, but also look at the rest of the text i posted above in the entry for 981 :
 +
  Quanz et al. (2007, ApJ, 656, 287, also astro-ph/0610786 -- see http://arxiv.org/abs/astro-ph/0610786 for free
 +
  copy of paper) [...] One of the questions they address in this paper is whether or not V1331 Cyg formed on its own,
 +
  or with 'friends.' They talk in their paper (see sections 4.2 and 4.3) about whether some objects found in the LDN
 +
  black parts are real YSOs or not, and they conclude based on available evidence that they are not YSOs. BUT, maybe
 +
  they just weren't looking in long enough wavelengths. We might find that these stars really are YSOs... or we may
 +
  not. We may confirm that yes, they are just foreground objects superimposed on the dark lanes of the nebula.
 +
 
 +
--[[User:CJohnson|CJohnson]] updated 9:00 CDT 02 May 2008
 +
=Travel Arrangements=
 +
If you want to e-mail me your travel arrangements, I would be happy to update this chart.
 +
 
 +
{| border="1"
 +
|LDN
 +
|Pete
 +
|Chelen
 +
|David
 +
|John
 +
|Cris
 +
|Tim
 +
 
 +
|-
 +
|Arrival date/time
 +
|13-June, 20:08 (LAX) Delta 79
 +
|13-June, 20:15 (BUR)
 +
|13-June
 +
|13-June, 11:55 (BUR) Canadair 2836
 +
|13-June, 15:05 (BUR)
 +
|x
 +
|
 +
|-
 +
|# of students (male/female)
 +
|1/1
 +
|0/0
 +
|1/2
 +
|0/0
 +
|2/0
 +
|yes
 +
 
 +
|-
 +
|Hotel**
 +
|HIE
 +
|HIE
 +
|HIE
 +
|HIE
 +
|HIE
 +
|x
 +
|
 +
|-
 +
|Auto rental??
 +
|yes, car
 +
|no
 +
|personal car
 +
|no
 +
|no
 +
|yes, van
 +
|
 +
|-
 +
|Departure date/time
 +
|17-June 22:50 LAX Delta 648
 +
|18-June 7:15
 +
|19-June
 +
|18- June 11:17 LAX United 5435
 +
|18-June
 +
|x
 +
|}
 +
 
 +
**HIE=Holiday Inn Express-Pasadena, BW=Best Western Pasadena Royale
 +
 
 +
Peace,
 +
--chj
 +
[END]

Latest revision as of 14:04, 2 May 2008

I haven't done this legwork yet because I thought you might want to be involved - finding a good target for observation is a substantial part of doing science! :)

Ideally, we'd pick a target for our observation using a combination of

  • searching ADS and/or SIMBAD for existing literature .... we want something that doesn't have a LOT of other references, but some references are fine - if someone else has already assembled data on an object, we might be able to use those data and/or results - we just don't want something that has already been "done to death." (page from the wiki on literature searching)
  • checking POSS and other existing multi-wavelength data to see what the object looks like in those bands .... does it look thick and dark in the optical? bright in the infrared? Both of those things suggest that it will be interesting with Spitzer. Something that looks diaphanous in the optical will likely turn out to be completely transparent with Spitzer. (page from the wiki on introduction to data at other wavelengths; you can also do this with Leopard -- see next item.)
  • and, checking to see if it is or is not in the Spitzer archive .... you need to use Leopard to do this. (page from the wiki on searching the archive using Leopard-- NB: "searching the archive to see what is there" is the same thing as "downloading data" except that when you search to see what is there, you don't actually download the data, you just see that there is something there.) Also, note that just because there is data already in the Archive on a given cloud doesn't mean it's a BAD thing, just that it's not a good thing for a new proposal. You should make a note of the "nice" ones you find, because you can go grab the data as soon as the data are public.


My original thoughts on good targets were the following three: LDN 470, LDN 1225, LDN 880 (but maybe too diaphanous). And, at the AAS, you guys also came up with LDN 1340.

General information re: lists of targets

The master list of objects that I worked from is here, courtesy of Babar Ali. Note that these are all opacity class 5 objects. Opacity class 5 or higher is what we probably want for Spitzer observations. None of these have many references in ADS. This is not meant to be a comprehensive list by any means, just a place to start. If you want to instead start with the complete Lynds Dark Nebulae catalog, it's here (the data are linked as "online data" or something similar).

Please post your thoughts and reactions to each of these targets, and any new ones you think are viable candidates for observation. For example, you might post a gif or jpeg of the POSS image you found, or a summary list of references (e.g., "3 papers besides Lynds, one radio, others submm" or whatever). Note the syntax I'm using to post comments on LDN 1340 below -- this is a method suggested by the Oil City folks, and I think it works really well to follow the conversation. See the help page linked from the left (above the search box) for hints on how do this.

--Guastella 20:48, 8 January 2008 (PST) Here is the article I mentioned in our meeting earlier today. (this is the one that looked in radio at optically-selected cores and reported which ones were "empty.")

THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 123:233È250, 1999 July (1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. A CATALOG OF OPTICALLY SELECTED CORES CHANG WON LEE AND PHILIP C. MYERS [...] This didn't format well. Please let me know if there is a better way to send papers Thanks Pete [END]

(--Rebull 09:25, 9 January 2008 (PST) he's right, this didn't format well, so I replaced it with a link directly to ADS, from which you can get the complete article - there's no access restrictions on it, and if you go there, you can get the originally formatted PDF or the html. ADS link to the Lee and Myers paper [END] )

--Rebull 13:44, 14 January 2008 (PST) David added some general target selection stuff to the talk page [END]

--Rebull 07:55, 18 January 2008 (PST) weeding down a big target list - step-by-step, what I did to weed down the full Lynds target list. [END]

Observing time

--Rebull 13:59, 14 January 2008 (PST) David asked re: time to cover area. A map I have here that goes about the depth we want covers about 0.6deg x0.6 deg with IRAC takes 1.5 hrs, and more or less the same area takes another 1.4 hrs with MIPS. 3 hrs is probably too much to ask for, especially if you want to ask for more than one cloud. less than that size, 0.3 deg x 0.3 deg, with IRAC takes 0.4 hrs, and up to 0.7 hrs with MIPS. (i can get clever and try to make that less time, but this is the lowest-energy solution.) For an irregularly-sized thing like LDN 951, i can get creative and make something other than a square map, but it takes longer for me to design. so we need to decide if (a) we have something really cool we want to completely map, or (b) two smaller things (could be pieces of a large thing) we want to map to compare them. Note that, for example, the object LDN 1340 is more like ~1 degree x ~1 degree, so we'd have to do just a small piece (or two small pieces) of it. [END]

LDN 470

Ldn470possred.gif LDN 470 in POSS-red. image is 0.25 deg on a side. --Rebull 14:09, 14 January 2008 (PST)

--Mcdonald 15:39, 15 January 2008 (PST) Hi, here is a colored image of LDN 470: 

  Ldn470.jpg

LDN 1225

Ldn1225possred.gif LDN 1225 in POSS-red. image is 0.25 deg on a side. --Rebull 14:09, 14 January 2008 (PST)

--Mcdonald 15:44, 15 January 2008 (PST) Here is a 15 arcmin x 15 arcmin colored image of ldn1225: 

  Ldn1225.jpg

LDN 880

Ldn880possred.gif

LDN 880 in POSS-red. image is 0.25 deg on a side. Still a little worried that this is too optically thin to make a good Spitzer image. but maybe we could focus very specifically on the dark thing to the southwest.

--Rebull 14:09, 14 January 2008 (PST)

Deepi.png Deepr.png - LDN 880, about the same scale, in relatively deep I and R from the USNO 1.0m. --Rebull 14:43, 14 January 2008 (PST)

--Mcdonald 15:47, 15 January 2008 (PST) Here is John's colored image made in Austin again 15 x 15 arcmin: 

  LDN880 by John.jpg

LDN 1340

Ldn1340possred.gif

LDN 1340 in POSS-red. image is 0.25 deg on a side. --Rebull 14:09, 14 January 2008 (PST)


--Rebull 20:14, 8 January 2008 (PST) Here's a summary of the latest developments on this object:


One of you (Peter?) suggested this object - and it was a fabulous suggestion. Beautiful in the optical, with IRAS sources, a handful of existing literature, and no Spitzer. Perfect! The icing on the cake was that it's visible in the Spring.

One of you (Peter again?) noticed that there was another AAS poster from 2005 on this object. I mentioned that I knew 2 of the authors (JoAnn O'Linger and Grace Wolf-Chase). Not 2 hours after leaving you, I ran into them. One thing I didn't mention in the context of searching the archive is that there is an open call for proposals out now, eg., there are ~700 proposals for objects that are currently being reviewed, and 20% of them will get their targets approved by March. To some extent, since you're putting in a proposal more or less now, you kind of trump them. On the other hand, it's never good to make enemies.... So, it turns out that JoAnn and collaborators have submitted a proposal to map this region over 1 square degree. There's no guarantee that their data will actually be taken this cycle (before we run out of cryogen in Spring 2009), but at the same time, we probably won't be able to ask for a full square degree (it would take too much time). We could pick a subregion to focus on, or we could find another target entirely.

I'll continue to talk to JoAnn (we had just a brief conversation today), and if I can get her posters (one from before, one from this meeting!), I'll post them here.

[END]


--Guastella 20:48, 8 January 2008 (PST) In case we are still looking at this here is the 2005 Abstract Submillimetre Observations of an Intermediate-Mass Star Forming Cloud Core J. O’Linger, G. H. Moriarty- Schieven, and G. A. Wolf-Chase

ADS link to AAS abstract

ADS link to PPV abstract

--Rebull 09:37, 9 January 2008 (PST) I talked to JoAnn again today, and she thinks that maybe doing just a piece of the cloud would be a good idea. She showed me some of her supporting data, and indeed this is a really cool area. We could do just a part of it now, and eventually, she'll map the rest of the cloud as well.

Here's her poster from today: Media:joann2008poster.pdf

[END] --Mcdonald 15:51, 15 January 2008 (PST) 15 x 15 colored image: 

  Ldn1340.jpg

LDN 951

From: cdewolf@chsd.us How does LDN 951 look? Assuming I did my query right, it also hasn't been looked at by Spitzer. I found it on a list of LDNs that have visual opacities of 6 in a paper by Visser et. al, 2002. There's another, but it doesn't look as interesting. Cris L. DeWolf LDN951.red.jpg


--Rebull 14:00, 9 January 2008 (PST) ooh, this is a nice one! you're right, it doesn't have any Spitzer observations yet. This might very well be a good candidate! [END]

--Dewolf 06:00, 12 January 2008 (PST)There was a study of IRAS associations with dark clouds (Parker, N.D., 1988) that appears to indicate a good chance of there being a YSO in LDN 951. Here's a link to the article. [1] [END]

--Mcdonald 15:54, 15 January 2008 (PST) A 15 x 15 arcmin colored image: 

  Ldn951.jpg

Other targets

--Rebull 11:42, 9 January 2008 (PST) I found two posters today on Lynds clouds - L1221 and L988e. L1221 has Spitzer data which is pretty cool; L988 doesn't have any Spitzer data. Take a look at the other bands and references and see if it would be interesting.... [END]

--Rebull 14:09, 14 January 2008 (PST) nevermind; the L988 image is pretty much just a star field. [END]

L1014.jpg

--Rebull 14:27, 14 January 2008 (PST) just for comparison, here is a spitzer composite image of L1014. we'd be very lucky to find something like this, but this is the hope. [END]

--Rebull 13:44, 14 January 2008 (PST) David added some general target selection stuff to the talk page [END]


--Rebull 10:48, 15 January 2008 (PST) Out of David's top 16 suggestions, the only ones wihtout existing spitzer data are ldn 1357 (right on the edge of some existing spitzer data) and ldn 1358. you must be doing something right, as you're hitting popular objects. ;) [END]

--Rebull 14:19, 21 January 2008 (PST) but really from jan 20: tim sent this in email: 

  I have been doing some looking at the Lynds targets.  I'm attaching pics of LDN 1598 and LDN 1340.  
  I could not find anything in ADS about either of these targets, so it looks like they have not been 
  studied a great deal.  I like the fact that you have a dark area next to a fairly rich star field 
  (especially with 1598).  This would tend to indicate a dense nebulous area.  the images are 5'x5'. (targets suggested by Tim Spuck)

here's the graphics: (L1598 first, then L1340): Tim l1598.jpg Tim l1340.jpg

--Rebull 14:26, 21 January 2008 (PST) actually, i get 19 references for ldn 1598, and 15 for L1340, both using simbad... [END]

--Spuck 05:37, 22 January 2008 (PST) Luisa, just for future reference, I thought ADS was a more complete database for identification of current research. I assume this is not the case since you found many references in simbad. Is that correct? Thanks, Tim [END]

--Spuck 06:57, 22 January 2008 (PST) Ok ... I think I may have answered part of my question. I was seaching on LDN1598 and coming up with nothing, but if I search on L1598 or L1340 I am at least coming up with something in ADS (one for 1598, and seven for L1340). I need to play with the parameters a bit. [END]

--Rebull 17:57, 22 January 2008 (PST) they're different sorts of databases, with different strengths and weaknesses. ADS is driven by the literature itself, whereas SIMBAD is driven more by object lists. ADS is usually more complete. But, for example, some of the references for L1685 don't actually call it L1685 anywhere in the paper. ADS may or may not have the information that those papers really do have data about that object - sometimes ADS knows, and sometimes ADS doesn't. Someone at the SIMBAD end did realize (or at least THINKS) that the objects are the same, and has (hopefully correctly) tied the object to the paper. SIMBAD often requires a human to make the association between synonyms for certain objects, and this can be fallible, especially for the more obscure objects. ADS is generally more accurate in the following sense - SIMBAD may quote a spectral type, but to be sure that whatever object you are looking at really has that type, track down the original papers and make sure that the actual original paper really does cite that type. More obscure papers are rarely in SIMBAD, but they can be found in ADS. ADS and SIMBAD are heavily interlinked, so there's a lot of ways to get between them. [END]

--Dewolf 22 Jan 2008 10:19:06 (question submitted via regular email): I'd seen some images [before] with the large pixel areas as well. How do you find a potential IRAS source in a small LDN with such poor resolution? [END]

--Rebull 10:19, 22 January 2008 (PST): Your question really has a two-part answer.

The first part is that I'm not detecting sources by eye. I'm relying upon the computer-generated IRAS Point Source Catalog (PSC) and Faint Source Catalog (FSC) which are described along with the rest of the IRAS mission information here: http://irsa.ipac.caltech.edu/IRASdocs/iras.html

If you get into the documentation, you will find that the catalog consists of, among other things, measurements at each of the 4 IRAS wavelengths, and a quality flag for each of the 4 bands. This quality flag is REALLY IMPORTANT, as it tells us whether the computer thought it was a real detection at each band, or just an upper limit at a particular band. Because the resolution of IRAS is so poor, indeed, it can be fooled.

One of the objects in our shortlist below really did have a recognizable clear point source right on the center of the object at 25 um. But, the rest, I agree, I'd be hard-pressed to identify the source by eye. That doesn't mean it's not there, however. The computer is really good at finding real, faint sources. When we go to write this up, we really should pay attention to whether the computer felt it was a point source just at 100 um and not at 12 or 25 um. For this subset of objects, I am cheating a little because several of them have observations at other wavelengths, enough so that I know there's a real source there, so I didn't go check the quality flags for those objects.

The second aspect of the answer is that when we go look with Spitzer, it could very well be that the source dissolves away into background nebulosity, or breaks into pieces. We have an image at 24 um of something in the Perseus star-forming region that appears in the IRAS catalog as a single object, IRAS 03388+3139. But, when we look with Spitzer, it breaks up into 9 objects. This stuff appeared in Rebull et al., 2007, ApJS, 171, 447 (also findable in astro-ph, look near Jan 2007), along with an analysis of what IRAS sources dissolved away completely into nebulosity when viewed with Spitzer. The nebulosity is very complex here, so it happens. [END]

A (The?) Shortlist

Goal: find anywhere from one to a few LDN likely to host young stars so that we not only have a pretty picture but also find some new baby stars. If we are going to ask for more than one cloud, they need to have different properties, so that we can explain that we are looking at THIS sort and THAT sort to compare. And we can (should) also say we will mine the Spitzer archive for more examples.

Luisa's Favorites

LDN Image Notes
951 Ldn951 possred.jpg (POSS/Red, 0.25 deg on side)
  • from cris (see above.)
  • opacity class 6 (good, deep and dark)
  • 'linear' (as opposed to 'blobby')
  • (Visser et al. 2002, AJ, 124, 2756) part of the cygnus rift, 700 pc away, max extinction Av=10, just 4.7 Msun in cloud
  • IRAS source 21186+4320
  • (ref?) two submm 'starless cores' here : in 1950 coordinates 21:18:20 +43:19:17 and 21:18:22.9 +43:19:51 -> we might not find anything, but we might find some of the youngest stars forming here.
  • visible to spitzer through tomorrow 1/22 (argh!); next window june 27-sep 10.
  • IRAC total time 907 sec, MIPS total time 3313 seconds. IRAC: media:ldn951_withirac.gif (irac has two fields of view, portrayed by the two colors; the region covered by both colors is the region we'll get with all 4 irac bands [3.6, 4.5, 5.8, and 8 um]. note that the specific portion of sky that we will cover rotates, so these observations are designed to catch as much of the LDN as i can and still be independent of rotation angle.) MIPS: media:ldn951_withmips.gif (MIPS has 3 cameras, but we're only using 2 -- indicated by the two colors, 24 and 70 um.
  • with irac we will see mostly stars, some nebulosity. we need at least MIPS-24, which is 1191 seconds of the 3313 seconds; mips 24 will help us find stars, but also find the nebulosity. in this specific case, where we have some submm cores, mips70 is important too, as it might be just at mips70 that we see these submm cores. note that i get a little too much sky at 24 and not quite enough at 70; i'm constrained by the choices i have in the AOR construction, and i'm optimizing for science and time, not necessarily a pretty picture.
  • TOTAL TIME: 1.2 hrs. (4 IRAC plus 2 MIPS)
425 Ldn425 possred.gif (POSS/Red, 0.25 deg on side)

Ldn425 mycenter possred.gif

  • from cris' ppt based on some subset of my target weeding.
  • opacity class 5 (good, pretty deep and dark)
  • 'blobby' (as opposed to 'linear')
  • Lee and Myers (1999, ApJS, 123, 233) find a YSO here (1950 coords: 17 44 15.4 −04 34 07)
  • IRAS source 17442−0433
  • Connelley et al (2007 AJ 133, 1528) find a new NIR reflection nebula here, suggestive that a YSO is illuminating the nebula, and that we will see something pretty at IRAC bands.
  • the part that is the center of the coordinates given by lynds (center of image at left) seems offset from the darkest part as seen in POSS. X's in graphic at left are the IRAS point sources in this region; the northernmost one is the one listed in the literature. there is not much to the dark cloud north of the image region shown at left. I'm taking as the center 17:46:55 -04:36:25; see second graphic at left.
  • visible to spitzer apr 12-may 23, then sep 21-nov 2.
  • IRAC total time 657 seconds (media:ldn425_mycenter_possred_withirac.gif) MIPS-24 total time only 395 seconds. Harder to justify 70 um time too here, since it will be expensive and it's not entirely clear what we will see. Could simply plan to jump on the data right away and ask for more time to do 70 if it seems likely to be interesting. (media:ldn425_mycenter_possred_withmips.gif - box is "my center" for this observation and x's are IRAS sources.)
  • TOTAL TIME: 0.3 hrs. (4 IRAC plus 1 MIPS)
981 Ldn981 possred.gif (POSS/Red, 0.3 (not 0.25!) deg on side)
  • from cris' ppt based on some subset of my target weeding.
  • opacity class 6 (good, deep and dark)
  • 'linear' (as opposed to 'blobby')
  • Quanz et al. (2007, ApJ, 656, 287, also astro-ph/0610786 -- see http://arxiv.org/abs/astro-ph/0610786 for free copy of paper) has a very interesting article about the structures around V1331 Cyg, a known YSO. They were studying the immediate environment of this thing using HST, but it is at the end of one of the filaments associated with LDN 981. One of the questions they address in this paper is whether or not V1331 Cyg formed on its own, or with 'friends.' They talk in their paper (see sections 4.2 and 4.3) about whether some objects found in the LDN black parts are real YSOs or not, and they conclude based on available evidence that they are not YSOs. BUT, maybe they just weren't looking in long enough wavelengths. We might find that these stars really are YSOs... or we may not. We may confirm that yes, they are just foreground objects superimposed on the dark lanes of the nebula. V1331 Cyg is just on the edge of the image, to the upper left, at the end of that dark lane, with the funny circular bright nebula (that was what Quanz et al studied with HST).
  • image from tim comparing more wavelengths
  • image from cris comparing scales
  • visible to Spitzer through jan 27 (argh!), then june 26-feb 3 (not a typo, nice and long!)
  • some existing MIPS data to the east (left) and north (up) which we could grab and add in to our maps.
  • IRAC total time 2152 sec (media:ldn981_possred_withirac.gif) **need to add a constraint to both IRAC and MIPS that it be done before sep 15 (1 for MIPS) in order to cover the region we want. (usually constraints are bad, but i'd have to ask for more time otherwise, and we are giving them a large window, so it should be ok.) MIPS 24 only 1191 sec. (media:ldn981_possred_withmips24.gif) Again, somewhat hard to justify asking for 70 um time, but this time, V1331 Cyg is an IRAS source, so maybe worth it. MIPS-70 alone is another 6079 sec. (!) (media:ldn981_possred_withmips70.gif)
  • TOTAL TIME: 0.9 hrs (4 irac plus 1 mips) or 2.6 hrs (4 irac plus 2 mips)
1143 Ldn1143 possred.gif (POSS/Red, 0.3 deg on side - now spot won't let me do 0.25, ??)
  • from cris' ppt based on some subset of my target weeding.
  • opacity class 6 (good, deep and dark)
  • 'blobby' (as opposed to 'linear')
  • Lee and Myers (1999, ApJS, 123, 233) find a YSO here (1950 coords: 21 57 03.0 58 42 25)
  • IRAS source 21569+5842
  • Connelley et al. (2007 AJ 133, 1528) find a new NIR reflection nebula here, suggestive that a YSO is illuminating the nebula, and that we will see something pretty at IRAC bands.
  • Magnier et al. (1999, A&A, 352, 228) find something they call a "transition object" here, and is noted specifically as a "very red star." It's likely we will be better able to tell what this thing is.
  • visible to Spitzer through feb 22 (too soon to schedule us) and then jul 23-mar 2 (again, not a typo, nice and long).
  • IRAC total time 907 sec (media:ldn1143_possred_withirac.gif - box is 'target', x's are iras sources), MIPS-24 total time 1191 sec (just mips24, not mips70 too, again hard to justify) (media:ldn1143_possred_withmips24.gif).
  • TOTAL TIME: 0.6 hrs (4 irac plus 1 mips)
1598 Ldn1598 possred.gif (POSS/Red, 0.3 deg on side - now spot won't let me do 0.25, ??) x's are IRAS sources
  • from Tim based on some subset of my target weeding
  • opacity class 5 (good, pretty deep and dark)
  • 'blobby' (as opposed to 'linear')
  • 19 refs in SIMBAD.
  • IRAS 05496+0812, also WB89 718, also HH 117 VLA 1 (so clearly several people have looked here before). This is part of the lambda Ori complex, apparently, and maybe related to alpha Ori (Betelgeuse). There is a lot of Spitzer data covering parts of the lambda Ori complex, but evidently not this cloud and its friend, L1599. I will ask my friends who are studying the lambda Ori complex about this object.
  • Wu et al. (2004, A&A, 426, 503) studied outflows and claim to find one here, placing the cloud at 0.9 kpc. Another paper, Hilton & Lahulla (1995, A&AS, 113, 325) cite Schwartz et al (1988) also at 900 pc.
  • Rodriguez & Reipurth (1998) find the exciting source for HH117 here; our observations as planned will also cover the HH object itself.
  • visible to spitzer mar 21-apr 29, then oct 18-nov 28.
  • IRAC total time 907 sec (media:ldn1598_possred_withirac.gif - box is 'target', x's are iras sources), MIPS-24 total time 1191 sec (just mips24, not mips70 too, again hard to justify) (media:ldn1598_possred_withmips24.gif).
  • TOTAL TIME: 0.6 hrs (4 irac plus 1 mips)
1685 Ldn1685 possred.gif (POSS/Red, 0.25 deg on side)
  • from Chelen based on some subset of my target weeding
  • opacity class 5 (good, pretty deep and dark)
  • 'blobby' (as opposed to 'linear')
  • 10 references in SIMBAD; aliases include BHR 157, [CB88] 73, Barnard 56, DCld 352.9+04.8
  • Huard et al. (1999, ApJ, 526, 833) does NOT detect this in the submm, and is able to constrain the distance at <160 pc (in front of the ophiuchus clouds).
  • I think it was also undetected by Bourke et al. (1995 MNRAS) in ammonia.
  • there is an IRAS source here; see x's in figure to left. IRAS 17056-3204 is the one closest to the center.
  • visible to spitzer apr 4-may 13 then sep 14-oct 24
  • IRAC total time 907 sec (media:ldn1685_possred_withirac.gif - box is 'target', x's are iras sources), MIPS-24 total time 1191 sec (just mips24, not mips70 too, again hard to justify) (media:ldn1685_possred_withmips24.gif).
  • TOTAL TIME: 0.6 hrs (4 irac plus 1 mips)

the AOR file to load into spot is here: media:lyndsaors.aor.txt - i had to add a ".txt" extension to get the wiki to accept it, but you should save the file to disk and rename it as just ".aor" and then Spot will recognize it as an AOR file.

Middle-of-the-road candidates

Usually they're just here because there's no good reason to reject them, but others seem prettier or more likely to host stars.

  • LDN 470 - small, opacity class=6.
  • LDN 1225 - bigger, opacity class 4 only (too thin?)
  • LDN 1125 - opacity class=5, blotchy/blobby, same as Barnard 152, Lee and Myers say YSO but appears in 'starless core' papers.
  • LDN 1139 - opacity class=5, blotchy/blobby, Lee and Myers say YSO but appears in 'starless core' papers.

Rejects, and reasons:

  • LDN 880 - lee and myers say no YSO; rather thin in optical images, and might just see through it in spitzer.
  • LDN 769 - lee and myers say no YSO; mentioned in several other "starless core" papers.
  • LDN 778 - many simbad refs (>40!) but most of them are 'starless core' papers
  • LDN 1041 - image looks like a plain star field
  • LDN 1082 - image looks like a plain star field
  • LDN 1340 - nice image, but consensus from the group was that they wanted to work in a 'new' region.

Voting and Ranking

If the editing of the table in the wiki intimidates you, or you're worried about making sure your vote appears under your column (this can be tricky), feel free to just email me your ranking, and I'll enter it here. "1" is high (most favorite), "6" is low (least favorite). So as not to bias you, I won't put in my votes until the very end.

LDN Pete Chelen David John Cris Tim Luisa AVERAGE
951 6 5 1 4 5 5 5 4.4
425 2 2 2 2 2 3 2.2
981 1 1 2 1 1 1 1 1.1
1143 3 4 3 5 3 4 2 3.4
1598 4 6 3 4 3 4 4.0
1685 5 3 6 6 6 6 5.3

Rank-ordered list is therefore:

  • LDN 981 (rank 1.1) - 0.9 hrs spitzer time
  • LDN 425 (rank 2.2) - 0.3 hrs spitzer time
  • LDN 1143 (rank 3.4) - 0.6 hrs spitzer time
  • LDN 1598 (rank 4.0) - 0.6 hrs spitzer time
  • LDN 951 (rank 4.4) - 1.2 hrs spitzer time
  • LDN 1685 (rank 5.3) - 0.6 hrs spitzer time

I would counsel that you write a proposal for the top two clouds. They have some different properties, and the total time request of 1.2 hrs is not completely outrageous.

--Dewolf 08:54, 29 January 2008 (PST)The paper that Luisa referred to in her discussion of LDN 981 is worth a read as we prepare our proposal. Here is a direct link to a pdf of it media:0610786v1.pdf. The authors suggest that V1331 Cyg evolved from one of the filaments in this linear cloud. To me, this implies a strong possibility of additional YSOs in the cloud. What do you think? [END]

--Rebull 13:02, 30 January 2008 (PST) Yep, i think it's a strong possibility, but also look at the rest of the text i posted above in the entry for 981 : 

  Quanz et al. (2007, ApJ, 656, 287, also astro-ph/0610786 -- see http://arxiv.org/abs/astro-ph/0610786 for free 
 copy of paper) [...] One of the questions they address in this paper is whether or not V1331 Cyg formed on its own, 
 or with 'friends.' They talk in their paper (see sections 4.2 and 4.3) about whether some objects found in the LDN 
 black parts are real YSOs or not, and they conclude based on available evidence that they are not YSOs. BUT, maybe 
 they just weren't looking in long enough wavelengths. We might find that these stars really are YSOs... or we may 
 not. We may confirm that yes, they are just foreground objects superimposed on the dark lanes of the nebula.

--CJohnson updated 9:00 CDT 02 May 2008

Travel Arrangements

If you want to e-mail me your travel arrangements, I would be happy to update this chart.

LDN Pete Chelen David John Cris Tim
Arrival date/time 13-June, 20:08 (LAX) Delta 79 13-June, 20:15 (BUR) 13-June 13-June, 11:55 (BUR) Canadair 2836 13-June, 15:05 (BUR) x
# of students (male/female) 1/1 0/0 1/2 0/0 2/0 yes
Hotel** HIE HIE HIE HIE HIE x
Auto rental?? yes, car no personal car no no yes, van
Departure date/time 17-June 22:50 LAX Delta 648 18-June 7:15 19-June 18- June 11:17 LAX United 5435 18-June x
    • HIE=Holiday Inn Express-Pasadena, BW=Best Western Pasadena Royale

Peace, --chj [END]

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