Jackie BRC 38 - Revision history

Barge at 23:20, 5 March 2012

2012-03-05T23:20:02Z

Barge at 23:03, 5 March 2012

2012-03-05T23:03:18Z

Barge at 19:30, 5 March 2012

2012-03-05T19:30:20Z

Barge at 18:09, 5 March 2012

2012-03-05T18:09:36Z

Barge at 17:46, 5 March 2012

2012-03-05T17:46:01Z

Barge at 17:44, 5 March 2012

2012-03-05T17:44:41Z

Barge at 16:59, 5 March 2012

2012-03-05T16:59:14Z

Barge at 08:02, 5 March 2012

2012-03-05T08:02:45Z

Barge at 08:00, 5 March 2012

2012-03-05T08:00:34Z

Barge at 07:59, 5 March 2012

2012-03-05T07:59:17Z

@@ Line 20: / Line 20: @@
 BRC 38 has been observed with IPHAS, Spitzer, and 2MASS surveys (Barensten et al 2011; Choudhury et al 2010; Beltran et al 2002). A survey with VLA and BIMA (Beltran et al 2002) found three intermediate-mass YSO sources in different stages of evolution. A Chandra x-ray study found over one hundred x-ray sources in IC 1396N using the Chandra ACIS detector (Getman et al. 2006).  About a quarter of those are associated with YSOs, representing a variety of stages (transitional Class 0/I protostar, Class I protostars, transitional Class I/II star, Class II classical T Tauri stars and Class III T Tauri stars). One of the youngest sources detected in x-ray, #66, is found close to the source IRAS 21391+5802 (Getman et al. 2006).<br>
 IRAS 2139+5802 has been studied in the 3.1mm radio wavelength  with PdBI, the Plateau de Bure Interferometer. Two areas in IC1396N are distinguished: 1. YSOs at the BIMA 3 location and the protocluster BIMA 2 location seen in dust continuum emission; and 2. filaments and clumps seen in molecular N2H emissions (Fuente et al  2009). BRC 38 has also been observed in H alpha emission, which is characteristic of young low mass stars. Nakano et al (2012) found 5 of Getman’s x-ray sources in BRC 38 matched H alpha stars they observed.
 <br><br>

@@ Line 15: / Line 15: @@
 : radio (IRAM & BIMA)
 : x-ray
-<br>
+<br><br>
 ==Draft Proposal==
-. What is the structure of brc 38?  - classification of cloud (type A I believe) & why; H2 jets and Herbig-Haro objects & what they indicate; <br>
+Bright Rimmed Cloud 38 is located in the H2 region IC 1396. Since it is located in the northern part of IC 1396 is it often referred to as IC 1396N.  It has a C shape with the southern edge as the brightest part (Pottasch et al. 1956). Ogura et al (2002) mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs. Intermediate mass protostars have been found there, though some (Ogura & Sugitani 1999) suggest there is probably a lot of low mass formation going on too. Wang et al. 2009 believes there is also potential for high mass stars formation.  H2 jets were found (Saraceno et al. 1996; Nisini et al. 2001)  as well as Herbig-Haro objects (Repurth et al. 2003; Nisini et al 2001). The Infrared Astronomical Satellite (IRAS) located the strongest source at 21391+5802, also known as BIMA 2, that is thought to be a low mass Class 0 source (Beltran et al. 2002, 2004).  This source has H2 emission in the form of bow shocks (Connelley, et al. 2006). These characteristics indicate this source is young object (Beltran et al 2002).<br>
-. What is the distance of the brc?
+BRC 38 has been observed with IPHAS, Spitzer, and 2MASS surveys (Barensten et al 2011; Choudhury et al 2010; Beltran et al 2002). A survey with VLA and BIMA (Beltran et al 2002) found three intermediate-mass YSO sources in different stages of evolution. A Chandra x-ray study found over one hundred x-ray sources in IC 1396N using the Chandra ACIS detector (Getman et al. 2006).  About a quarter of those are associated with YSOs, representing a variety of stages (transitional Class 0/I protostar, Class I protostars, transitional Class I/II star, Class II classical T Tauri stars and Class III T Tauri stars). One of the youngest sources detected in x-ray, #66, is found close to the source IRAS 21391+5802 (Getman et al. 2006).<br>
-. What is known about YSO in this region - this might be H alpha emission stars (??); <br>
+<br><br>

@@ Line 81: / Line 81: @@
 | Wang et al. 2009||The relation between 13CO j=2-1 line width in moelcular clouds and bolometric luminosity of associated IRAS sources||'''Luisa adds:'''  Radio. ignore at least for now<br>IRAS 21391+5802 - suggests that it is a star forming cluster where high-mass stars will form||http://arxiv.org/pdf/0909.3312v1.pdf
 |-
-| 6. <br>Chauhan et al. 2009 <br> <br> ON LAST YEAR'S LIST||Triggered star formation & evolution of t-tauri stars in and around BRC||'''Luisa adds:'''  YES this is a useful paper -- they are using JHK to select YSOs and including IRAC (but not MIPS) in their assessment of youth. we will be using longer-wavelength infrared to find the objects, so we will find a different set of objects. (ps they also didn't do that hot a job with source matching to the literature. we can do better.)<br>Study that looked at ages of star forming clusters. Seems to have a lot of background material on BRC 38. <br>'''Jackie adds:''' 2MASS and Spitzer-IRAC data was used to support BVIc observations. 18 YSOs were observed and analyzed. There is an age gradient, with younger stars on the inside of the rim or on the rim itself and older stars outside of it. ||[http://arxiv.org/pdf/0903.2122v1.pdf 2009, MNRAS, 396, 964]
+| 6. <br>Chauhan et al. 2009 <br> <br> ON LAST YEAR'S LIST||Triggered star formation & evolution of t-tauri stars in and around BRC||'''Luisa adds:'''  YES this is a useful paper -- they are using JHK to select YSOs and including IRAC (but not MIPS) in their assessment of youth. we will be using longer-wavelength infrared to find the objects, so we will find a different set of objects. (ps they also didn't do that hot a job with source matching to the literature. we can do better.)<br>Study that looked at ages of star forming clusters. Seems to have a lot of background material on BRC 38. <br><br>'''Jackie adds:''' 2MASS and Spitzer-IRAC data was used to support BVIc observations. 18 YSOs were observed and analyzed. There is an age gradient, with younger stars on the inside of the rim or on the rim itself and older stars outside of it. ||[http://arxiv.org/pdf/0903.2122v1.pdf 2009, MNRAS, 396, 964]
 |-
 | Morgan et al. 2007 <br> <br> ON LAST YEAR'S LIST||A scuba survey of BRC||'''Luisa adds:'''  Radio. ignore at least for now<br> BRC 38 included in this study with SUBA data (submillimeter - microwave??); <br>Luisa's notes:  SCUBA submm survey (450+850 um) plus IRAS (12, 25, 60, 100 um), MSX, and 2MASS (erroneously identified as 2mm but really 2 micron). both 27 and 34 in here. next part of a PhD thesis. lots of nice overview, summary (as would be expected for a thesis) spread throughout article. seems to be a really long paper, but is almost all figures in the appendix. relevant issues: how the objects they are talking about (at long and short wavelengths) compare to what we see in our images (see Resolution and their, e.g., fig 4). Forward reference to Spitzer data analysis like ours but then says have already looked for GLIMPSE, 24 um obs. They are only looking at low-res flux densities. Appendix may be useful for scavenging additional targets if we want to do more analysis on more targets.||[http://arxiv.org/pdf/0711.0775v1.pdf 2008, A&A, 477, 557]

@@ Line 58: / Line 58: @@
 |-
-| 1a. <br>Nakano et al. 2012   ||Wide Field Survey of Emission-line Stars in IC 1396||Nakano reports a total of 639 Hα emission-line stars were detected in an area of 4.2 deg2 and their i′-photometry was measured. Their spatial distribution exhibits several aggregates near the elephant trunk globule (Rim A) and bright-rimmed clouds at the edge of the H ii region (Rim B and SFO 37, 38, 39, 41), and near HD 206267, which is the main exciting star of the H ii region.” || [[Media:Nagano_2012.pdf]]
+| 1a. <br>Nakano et al. 2012   ||Wide Field Survey of Emission-line Stars in IC 1396||Nakano reports a total of 639 Hα emission-line stars were detected in an area of 4.2 deg2 and their i′-photometry was measured. Their spatial distribution exhibits several aggregates near the elephant trunk globule (Rim A) and bright-rimmed clouds at the edge of the H ii region (Rim B and SFO 37, 38, 39, 41), and near HD 206267, which is the main exciting star of the H ii region.” <br><br>'''Jackie adds:'''H alpha emission is characteristic of young low mass stars because these emissions are characteristic of T Tauri stars. They found 5 of Getman’s x-ray sources in BRC 38 matched H alpha stars they saw. They suggest the primary mode of star formation in IC 1396 is the birth of low-mass stars associated with bright rims. Data charts and images showing locations included. || [[Media:Nagano_2012.pdf]]
 |-
@@ Line 77: / Line 77: @@
 | Morgan L. K., Urquhart J. S., Thompson M. A.,  2009 <br> <br>ON LAST YEAR'S LIST||CO observations towards bright-rimmed clouds||'''Luisa adds:'''  Radio. ignore at least for now<br> Luisa's old notes:  JCMT (CO) observations. both 27 and 34 in here. 22 arcsec resolution! (see Resolution and their fig 2 here.) Likely last of his thesis, or first of his postdoc. (Look, his address changed, so this was published while he was a postdoc, but it's the same collaborators as before at his old institution, so my guess it's leftover thesis work.) They think 27 has been triggered, 34 not; this provides a nice compare-and-contrast opportunity for our write-up. Quick read.||[http://cdsbib.u-strasbg.fr/cgi-bin/cdsbib?2009MNRAS.400.1726M 2009, MNRAS, 400, 1726]
 |-
-| 5. <br>fuente et al. 2009||Dissecting an intermediate-mass (IM) prostar||'''luisa adds:''' hm. very narrowly focused paper, seems to be just on one object and radio. was ready to say ignore it, but it is probably worth a quick skim to see if they mention anything substantive about the 'YSO BIMA 3' and 'cluster BIMA 2' mentioned in the abstract.<br>A  look at IRAS 21391+5802 emissions of N2H+, CH3CN, CS, BIMA (1.2mm & 3.1mm)<br><br>'''Jackie adds:'''IRAS 2139+5802 studied in radio wavelengths (PdBI – Plateau e Bure Interferometer) 3.1mm. Results were compared with older PdBI data (Neri et al. 2007) and BIMA data (Beltran et al 2002). Two areas in IC1396N are distinguished – 1. YSOs BIMA 3 and the protocluster BIMA 2 seen in dust continuum emission and 2. Filaments and clumps seen in molecular emission (N2H+).  Interestingly, they claim the ratio of [CH3CN] / [N2H+] is related to the spectral type of the star being formed because the ratio is a good measure of gas kinetic temperature. ||http://arxiv.org/pdf/0909.2267v1.pdf
+| 5. <br>fuente et al. 2009||Dissecting an intermediate-mass (IM) prostar||'''luisa adds:''' hm. very narrowly focused paper, seems to be just on one object and radio. was ready to say ignore it, but it is probably worth a quick skim to see if they mention anything substantive about the 'YSO BIMA 3' and 'cluster BIMA 2' mentioned in the abstract.<br>A  look at IRAS 21391+5802 emissions of N2H+, CH3CN, CS, BIMA (1.2mm & 3.1mm)<br><br>'''Jackie adds: '''IRAS 2139+5802 studied in radio wavelengths (PdBI – Plateau e Bure Interferometer) 3.1mm. Results were compared with older PdBI data (Neri et al. 2007) and BIMA data (Beltran et al 2002). Two areas in IC1396N are distinguished – 1. YSOs BIMA 3 and the protocluster BIMA 2 seen in dust continuum emission and 2. Filaments and clumps seen in molecular emission (N2H+).  Interestingly, they claim the ratio of [CH3CN] / [N2H+] is related to the spectral type of the star being formed because the ratio is a good measure of gas kinetic temperature. ||http://arxiv.org/pdf/0909.2267v1.pdf
 |-
 | Wang et al. 2009||The relation between 13CO j=2-1 line width in moelcular clouds and bolometric luminosity of associated IRAS sources||'''Luisa adds:'''  Radio. ignore at least for now<br>IRAS 21391+5802 - suggests that it is a star forming cluster where high-mass stars will form||http://arxiv.org/pdf/0909.3312v1.pdf

@@ Line 99: / Line 99: @@
 | 9. <br>Reipurth et al. 2003||Blowout from IC 1396N: The emergence of Herbig-Haro objects in the vicinity of bright-rimmed clouds||'''Luisa adds:'''  Reipurth et al usually work in Ha or forbidden emission lines to find HH objects. look to see if they have a list of objects in the region we care about, or if this is a more general paper.<br>Herbig-Haro flow (HH 777) found coming out of ic 1396N; located at 214041.6+581638<br><br>'''Jackie adds:''' IC 1396N were imaged with H alpha and S2 filters and four new HH flows were found, HH 777, 778, 779, and 780. While many near-infrared sources were found that apparently are young stars this study focused on the HH flows found. Computer modeling was used to find a match for observed features. No list of sources is included. (in IR, I think)||[http://iopscience.iop.org/1538-4357/593/1/L47/pdf/17405.web.pdf 2002, ApJ, 123:2597-2626]
 |-
-| 10. <br>Ogura, et el  2002 <br> <br> ON LAST YEAR"S LIST||Halpha emission stars and Herbig-Haro objects in and around BRC||'''Luisa adds:'''  YES this is useful - finding YSOs via Halpha<br> Part of Luisa's Notes from last year:  Most recent of the Sugitani series of four. Using Halpha to look for YSOs, following up their other work. relevant issues: using multiple wavelengths to find YSOs (see Finding cluster members), spatial resolution (see Resolution), caveats with finding candidates. Nice intro, summary of larger issues, discussion of results.<br><br>Looked for YSOs with H alpha emission. HH objects studied to learn more about their structure. Finder chart included for BRC 38 (also BRC 27 & 34) of 16 H alpha emission stars and data table with locations. Finder charts are also shown for HH objects in BRC 38.  They mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs. It should be studied in optical and IR.  ||http://iopscience.iop.org/1538-3881/123/5/2597/pdf/201506.web.pdf
+| 10. <br>Ogura, et el  2002 <br> <br> ON LAST YEAR"S LIST||Halpha emission stars and Herbig-Haro objects in and around BRC||'''Luisa adds:'''  YES this is useful - finding YSOs via Halpha<br> Part of Luisa's Notes from last year:  Most recent of the Sugitani series of four. Using Halpha to look for YSOs, following up their other work. relevant issues: using multiple wavelengths to find YSOs (see Finding cluster members), spatial resolution (see Resolution), caveats with finding candidates. Nice intro, summary of larger issues, discussion of results.<br><br>'''Jackie adds:'''Looked for YSOs with H alpha emission. HH objects studied to learn more about their structure. Finder chart included for BRC 38 (also BRC 27 & 34) of 16 H alpha emission stars and data table with locations. Finder charts are also shown for HH objects in BRC 38.  They mention that this cloud is extremely complicated, including multiple outflows and embedded YSOs. It should be studied in optical and IR.  ||http://iopscience.iop.org/1538-3881/123/5/2597/pdf/201506.web.pdf
 |-
 | 11. <br>Beltran  et al. 2002||IRAS 21391+5802: The Molecular Outflow and its Exciting source||'''Luisa adds:'''  this is probably worth looking at to see if there is anything point source-y in here.<br>VLA and BIMA observations of dust and gas surrounding IRAS source; 3 sources isolated with BIMA, each a YSO

@@ Line 87: / Line 87: @@
 | Neri et al. 2007||The IC 1396N proto-cluster at a scale of ~250 AU||'''Luisa adds:'''  radio. ignore for now at least.<br>observations in millimeter range to help develop understanding of formation of clusters vs individual star formation||http://arxiv.org/pdf/0705.2663v1.pdf
 |-
-| 7. <br>Getman et al. 2007||X-ray study of triggered star formation and protostars in IC 1396N||'''Luisa adds:'''  YES this is useful<br>x-ray sources in the globule of ic 1396N; good pictures to help with the visualization of 1396N and these sources; evidence of sequential star formation||http://arxiv.org/pdf/astro-ph/0607006v2.pdf<br><br>'''Jackie adds:''' A Chandra study that found 117 x-ray sources in IC 1396N. 25 are associated with YSOs. A variety of stages (transitional Class 0/I protostar, Class I protostars, transitional Class I/II star, Class II classical T Tauri stars and Class III T Tauri stars). One of the youngest sources detected in x-ray, #66, is found close to the source IRAS 21391+5802 (also called BIMA 2). List of these sources are included. These sources were matched against 2MASS and MIR data.  The authors believe there may be still undiscovered protostars because of the many massive luminous X-ray protostars found.
+| 7. <br>Getman et al. 2007||X-ray study of triggered star formation and protostars in IC 1396N||'''Luisa adds:'''  YES this is useful<br>x-ray sources in the globule of ic 1396N; good pictures to help with the visualization of 1396N and these sources; evidence of sequential star formation<br><br>'''Jackie adds:''' A Chandra study that found 117 x-ray sources in IC 1396N. 25 are associated with YSOs. A variety of stages (transitional Class 0/I protostar, Class I protostars, transitional Class I/II star, Class II classical T Tauri stars and Class III T Tauri stars). One of the youngest sources detected in x-ray, #66, is found close to the source IRAS 21391+5802 (also called BIMA 2). List of these sources are included. These sources were matched against 2MASS and MIR data.  The authors believe there may be still undiscovered protostars because of the many massive luminous X-ray protostars found. ||http://arxiv.org/pdf/astro-ph/0607006v2.pdf
 |-
 | Patel et al. 2007||Submillimeter array observations of 321 ghz water maser emission in cepheus a||'''Luisa adds:'''  Radio. ignore at least for now<br> No don\'t think there is anything here||http://arxiv.org/pdf/astro-ph/0702696v1.pdf
 |-
-| 8. <br>Connelley et al. 2006||Infrared Nebulae around Young stellar objects||'''Luisa adds:'''  check this to see if there is anything point source-y in here.<br> IRAS 21391+5802 - images show jet-like nebula and large patches of nebulosity||http://arxiv.org/pdf/astro-ph/0611634v1.pdf <br> <br>'''Jackie adds:''' IRAS located a source at 21391+5802 that is thought to be a low mass Class 0 source (Beltran et al. 2002, 2004).  This source has H2 emission in the form of bow shocks.
+| 8. <br>Connelley et al. 2006||Infrared Nebulae around Young stellar objects||'''Luisa adds:'''  check this to see if there is anything point source-y in here.<br> IRAS 21391+5802 - images show jet-like nebula and large patches of nebulosity<br> <br>'''Jackie adds:''' IRAS located a source at 21391+5802 that is thought to be a low mass Class 0 source (Beltran et al. 2002, 2004).  This source has H2 emission in the form of bow shocks.||http://arxiv.org/pdf/astro-ph/0611634v1.pdf
 |-
 | Valdettaro et al. 2005 <br> <br> ON LAST YEAR'S LIST||h2o maser emission from bright rimmed clouds in the northern hemisphere||'''Luisa adds:'''  Radio. ignore at least for now<br>H2O maser studied in brc 38; points to paper Valdettaro et al. 2005b which is supposed to be about analysis of BRC 38. <br>  Luisa's old notes: 22.2 GHz (=1.35 cm if I did my math right). Really nice intro summarizing the big picture. Following up on Morgan and similar work asserting high-mass stars forming in BRCs by looking for masers. Our objects observed, not detected. Finding lots of non-detections, suggesting that low-mass stars forming instead. Nice, short writeup of basically a non-result, and I think they've gotten the interpretation spot-on. ||[http://arxiv.org/pdf/astro-ph/0508446v1.pdf 2005, A&A, 443, 535]
@@ Line 97: / Line 97: @@
 | Beltran et al. 2004||The dense moelcular cores in IRAS 21391 +5802 region||'''Luisa adds:'''  Radio and it sounds like theoretical models. ignore.<br> Three sources found with BIMA (??) observations in 21391+5802; Hard to read as they are trying to use data to fit/model how gas is emitted from the core||http://arxiv.org/pdf/astro-ph/0407102v1.pdf
 |-
-| 9. <br>Reipurth et al. 2003||Blowout from IC 1396N: The emergence of Herbig-Haro objects in the vicinity of bright-rimmed clouds||'''Luisa adds:'''  Reipurth et al usually work in Ha or forbidden emission lines to find HH objects. look to see if they have a list of objects in the region we care about, or if this is a more general paper.<br>Herbig-Haro flow (HH 777) found coming out of ic 1396N; located at 214041.6+581638 (in IR, I think)||[http://iopscience.iop.org/1538-4357/593/1/L47/pdf/17405.web.pdf 2002, ApJ, 123:2597-2626] <br><br>'''Jackie adds:''' IC 1396N were imaged with H alpha and S2 filters and four new HH flows were found, HH 777, 778, 779, and 780. While many near-infrared sources were found that apparently are young stars this study focused on the HH flows found. Computer modeling was used to find a match for observed features. No list of sources is included.
+| 9. <br>Reipurth et al. 2003||Blowout from IC 1396N: The emergence of Herbig-Haro objects in the vicinity of bright-rimmed clouds||'''Luisa adds:'''  Reipurth et al usually work in Ha or forbidden emission lines to find HH objects. look to see if they have a list of objects in the region we care about, or if this is a more general paper.<br>Herbig-Haro flow (HH 777) found coming out of ic 1396N; located at 214041.6+581638<br><br>'''Jackie adds:''' IC 1396N were imaged with H alpha and S2 filters and four new HH flows were found, HH 777, 778, 779, and 780. While many near-infrared sources were found that apparently are young stars this study focused on the HH flows found. Computer modeling was used to find a match for observed features. No list of sources is included. (in IR, I think)||[http://iopscience.iop.org/1538-4357/593/1/L47/pdf/17405.web.pdf 2002, ApJ, 123:2597-2626]
 |-
 | 10. <br>Ogura, et el  2002 <br> <br> ON LAST YEAR"S LIST||Halpha emission stars and Herbig-Haro objects in and around BRC||'''Luisa adds:'''  YES this is useful - finding YSOs via Halpha<br> Part of Luisa's Notes from last year:  Most recent of the Sugitani series of four. Using Halpha to look for YSOs, following up their other work. relevant issues: using multiple wavelengths to find YSOs (see Finding cluster members), spatial resolution (see Resolution), caveats with finding candidates. Nice intro, summary of larger issues, discussion of results. ||http://iopscience.iop.org/1538-3881/123/5/2597/pdf/201506.web.pdf