Why does this matter to you? (specific case of YSOs)
We spend a lot of time in the study of YSOs talking about the rings of dust around the young stars, and how they can become more prominent at longer wavelengths. When you look at the same object as seen with IRAC and MIPS, it will seem as if the source is getting larger at MIPS, and if the source is bright, it may even look as if it has a ring around it. See example here.
These two images are of the same tiny patch of sky, the left one using IRAC and the right using MIPS. Note that there are 'rings' around some of the sources seen in MIPS. THESE ARE NOT THE DUST RINGS AROUND THESE YOUNG STARS. I cannot emphasize this enough. There are only about 10 sources close enough to the Earth such that Spitzer can actually resolve the dusty disk. (here is one, Fomalhaut.) The sources you see in the little images here are not among those 10 close-by sources. What you are seeing here is the difference in resolution between IRAC and MIPS, and the (complicated) shape of the MIPS point-spread-function (PSF, or the way that the telescope+instrument+detectors respond to a point source of light).
The best way I can think of to explain features in the PSF that do not correspond to real, physical features is in pictures like this:
You know, from your own experience, that the lights on this football field are not really gigantic fuzzy blobs with funny purple halo/shadows lurking nearby. This is just how this camera+detector responded to this lighting situation, where these lights are very bright. Same thing in the astronomical images. There are features that are just a result of how the telescope+instrument+detectors respond to a point source of light, and these features are more prominent when the source is very bright.
When you are trying to match the same source across multiple bands, resolution matters. The apparently single point source that you see at 160 microns (or some other band, if you're grabbing non-Spitzer data from somewhere) may in fact combine flux from more than one source which is seen at IRAC bands. You have to be very careful in how you match up sources, assign flux matches for constructing SEDs, and/or apportion flux between two unresolved sources. For example, in theory, if there were two sources within the 160 um beam, you could put some fraction of the 160 micron flux to one source and some fraction to the other source within the beam. But what if the two sources are not the same brightness at 24 microns but they are at 8 microns? How do you decide how much of the 160 um flux to assign to one of the sources? These are complicated issues, and you need to investigate them for the sources you care about, and see if you need to worry about this for your objects.
Here is an example. The tiles are 3.6, 8, 24, 70, and 160 microns. Who gets that 70 micron flux? There's a 160 um flux there too but the PSF is bigger than the field of view. For that matter, who gets some of those 24 um fluxes? Ack!
When you are trying to find archival data for the same source, resolution matters. The apparently single point source that you see in your current data may not be appropriate to match to someone's catalog from 15 years ago. Catalogs created from images whose provenance you don't know should be used with caution. You should always try to put eyeballs on the original images if you can (not always possible).
Here is the same little patch of sky at POSS (blue, red, IR), COBE/DIRBE (some sort of combination of 1-100 um scans; yes, those are pixels), IRAS (12, 25, 60), WISE (3.4, 4.6, 12, 22 um), Spitzer (3.6, 4.5, 5.8, 8, 24, 70 um). Look how much the resolution matters. This is 2 point sources in the IRAS catalog (in some bands, you see only one source -- look at the location of the source at 12 compared to 60 -- this is not the same source!). The extended emission in the lower right at WISE is a much different shape than with Spitzer at comparable wavelengths.
What if you find a cool source that has the right colors to be a young star, and it seems to be a point source at all the bands you have? What if we go and check it in other bands? Guess what I'm gonna say: resolution matters. Here is a real-life example. This object was detected at WISE bands 1, 2, 3, and 4 (3.4, 4.6, 12, and 22 microns), and I found it as having the right colors to be a YSO. The first thing to notice is how the resolution changes when you go even from 12-22 microns, much less 3.4 to 22 microns. This is all on the same RA/Dec scale (e.g., the size of each tile in arcseconds is the same). Just stare at those four for a while. The rest of the tiles here are the same object, on the same scale, seen at 2MASS (JHK), POSS (blue, red, IR), and Sloan (ugriz). What was a point source to WISE is very clearly a nice little elliptical galaxy once you see it in SDSS (though, given its colors, it is probably not Elliptical, in the galaxy classification sense, but most likely it's an edge-on spiral with star formation going on). My color selection is successfully finding star formation, just not star formation here in our galaxy. (if you want to investigate this guy yourself, it's ra=76.8637916667, dec=25.51377778)
This one is a real exercise, in that you will need to go retrieve data, examine it, and think about it. In the CG4/Sa101 paper (Rebull et al. 2011, arXiv 1105.1180), we rejected source 073355.0-464838 as a YSO candidate because the flux density seen at 24 microns is likely contaminated by a nearby source at 8 um. Can you see this source in the images? Do you see why we dropped it? Should we have kept it?
Useful Related Links
Article on resolution from Bad Astronomy - this is in the context of debunking the moon hoax, but resolution issues are important for his discussion.
Another resolution discussion from Bad Astronomy.
Why can Hubble get detailed views of distant galaxies but not of Pluto? by Emily Lakdawalla at the Planetary Society
xkcd on angular size (link is actually to the explainer, which has more information than just the comic.
Questions to think about and things to try having to do with resolution
- What is the size of a typical HST image? How does it compare to a single Spitzer image, or a 'typical' Spitzer mosaic, or a single POSS plate, or the field of view of an optical telescope you have used, all compared with the size of the full moon? How does that compare to the size of a recent comet that visited the inner Solar System? or the size of a spiral arm of the Milky Way? You will have to go find on the web things like the field of view of these telescopes and these objects.
- Can you create a 3-color mosaic using just Spitzer data where the different resolutions of the various cameras is noticeable and important?
- Bonus question: how does the spatial resolution of all those telescopes listed above compare? (e.g., what is the smallest object you can resolve as more than a point source?)
- Are you going to laugh out loud the next time you're watching a crime drama, and someone says, "can you enhance that?" when referring to a blurry black-and-white image from a security camera, and someone else waves a magic wand and suddenly all sorts of small details are visible? (Can I wave my magic wand over that DIRBE image above and ever get that Spitzer/IRAC image?)
- C-WAYS Resolution Worksheet - developed in 2012 for the C-WAYS team
- C-CWEL Resolution Worksheet - developed in 2013 for the C-CWEL team
- HG-WELS Resolution Worksheet - developed in 2014 for the HG-WELS team
- IC 417 Resolution Worksheet - developed in 2015 for the IC417 team
- LLAMMa Resolution Worksheet - developed in 2016 for the LLAMMa team
- CephC-LABS Resolution Worksheet - developed in 2017 for the CephC-LABS team
- L1688 Resolution Worksheet - developed in 2018 for the L1688 team