b The flux for CrA-9 was computed using aperture photometry from the 70um
b  image; the catalog entry for this source shows it as a non-detection. 
b  CrA-9, located to the northwest of the Coronet region and TY CrA, has not
b  been previously observed, thus it is a new YSO candidate, classified as a
b  Class II. The source is located very close to the edge of the 70um map, so
b  there is no catalog entry in this band for it. However, the MIPS 70um image
b  clearly shows emission, and we estimate the flux using aperture photometry,
b  finding a 70um flux of 154.2+/-19.8mJy (using a 2 pixel aperture radius). 
c The flux for this source at this wavelength has been "band-filled"
c  (described in Section 3; in the c2d catalogs this is indicated as having an
c  image type of "-2"). Note that all these flux densities, flagged as
c  band-filled in our tables, should be considered as "bad photometry," like
c  the 5{sigma} upper limits in this catalog.
d This 70um flux is listed in the catalog with a "P" flag, meaning that there
d  were multiple catalog detections near this 70um source. The catalog source
d  chosen to match the 70um detection gave the most "consistent" SED, and was
d  also the one closest to the 70um detection (see the c2d Final Delivery
d  Document; Evans et al. 2007, Final Delivery of Data from the c2d Legacy
d  Project: IRAC and MIPS (Pasadena, CA: SSC)).
e In Table 13 of Fernandez et al. (2008A&A...480..735F), CrA-59 (RXJ1857.5-3732)
e  is referred to as a binary, where the eastern component has a spectral type
e  of M5 and the western component has a spectral type of M6. Only one source is
e  detected in our Spitzer observations. Note that this source does not have any
e  IRAC fluxes because it is off the field in the IRAC images (the MIPS field
e  extends a little further).
f Patten (1998ASPC..154.1755P) says this is not a member because it is an
f  eclipsing binary and if you work out the numbers, it is likely foreground.
f  This could be true because these are very bright fluxes.
g This flux is flagged "K" in the catalog meaning that it is complex, i.e.,
g  there are two or more detections within 2" in the same band in the same
g  epoch. The quality is likely still quite good, however.
j This flux has a quality of detection of "D" meaning it has a 2<=S/N<3.
j  Fluxes that do not have this note all have a quality of detection of "A"
j  (S/N>=7), "B" (S/N>=5), or "C" (S/N>=3).
k This flux is flagged "U" in the catalog indicating that it is an upper
k  limit because it has been band-filled and has an S/N<5.
l This flux has a quality of detection of "D" meaning it has a 2<=S/N<3.
l  Fluxes that do not have this note, in table 5, all have a quality of
l  detection of "A" (S/N>=7), "B" (S/N>=5), or "C" (S/N>=3).
m IRS 1 is the only source in this table that has a 70um flux in the 
m  catalog; it is an excellent "A" quality flux with a value of: 
m  33700.+/-4700.
n Discussed in Fernandez & Comeron (2001A&A...380..264F).
o This source is a double with CrA-54 (HD 176386B).
p This source name comes from Wilking et al. (1997AJ....114.2029W); it is
p  located to the northeast of source GP w (called GP wb in the same paper,
p  where GP is from Glass & Penston (1975MNRAS.172..227G) and was also seen by 
p  Walter et al. (1997AJ....114.1544W) who call the two sources CrAPMS 3 and 3B.
p  CrAPMS 3 is also a YSO candidate, and can be found in Table 6 as CrA-75.
p  It seems that in Meyer & Wilking (2009PASP..121..350M) there was some 
p  confusion when referring to GP wa - in that paper, it actually corresponds
p  to our CrA-75.
q Due to band-filling and saturation, the spectral index for R CrA has been
q  derived from the Ks and 5.8um bands alone. Its value and resulting
q  classification are likely incorrect. It should be noted that R CrA has
q  long been known to be a PMS star with an accretion disk (e.g., Knacke et
q  al. 1973ApJ...179..847K), and an SED slope of a Class II (Hillenbrand et al.
q  1992ApJ...397..613H).