J/A+A/551/A34 SED information for CrA members (Sicilia-Aguilar+, 2013)
Protostars, multiplicity, and disk evolution in the Corona Australis region:
a Herschel Gould Belt Study.
Sicilia-Aguilar A., Henning T., Linz H., Andre P., Stutz A., Eiroa C.,
White G.J.
<Astron. Astrophys., 551, A34-34 (2013)>
=2013A&A...551A..34S 2013A&A...551A..34S (SIMBAD/NED BibCode)
ADC_Keywords: Molecular clouds ; Stars, pre-main sequence ; Stars, late-type ;
Photometry, infrared ; Energy distributions
Keywords: stars: formation - stars: pre-main sequence - protoplanetary disks -
stars: late-type
Abstract:
The CrA region and the Coronet cluster form a nearby (138pc), young
(1-2Myr) star-forming region that hosts a moderate population of
Class I, II, and III objects.
We study the structure of the cluster and the properties of the
protostars and protoplanetary disks in the region.
We present Herschel PACS photometry at 100 and 160um, obtained as
part of the Herschel Gould Belt Survey. The Herschel maps reveal the
cluster members within the cloud with high sensitivity and high
dynamic range.
Description:
Broad-band continuum data were taken with the Photodetector Array
Camera & Spectrometer (PACS) on board the Herschel spacecraft. The
data were obtained as part of the Herschel Gould Belt Survey (Andre et
al., 2010A&A...518L.102A 2010A&A...518L.102A, see
http://gouldbelt-herschel.cea.fr/archives) in a similar way as the
rest of Gould Belt targets. Square scan maps with an extent of almost
89 arcmin on a side were obtained simultaneously in the 100 and 160um
filters on April 18, 2011.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
stars.dat 77 28 List of studied sources (table3, part 1)
table3.dat 74 290 SED information for CrA members (table3, part 2)
refs.dat 70 18 References
--------------------------------------------------------------------------------
See also:
J/A+AS/116/21 : Extinction toward CrA and Lup (Andreazza+, 1996)
J/A+A/475/959 : X-ray properties of young stellar objects (Forbrich+, 2007)
J/A+A/488/987 : Near-infrared survey of R CrA cloud (Haas+, 2008)
J/A+A/548/A24 : 1.3mm observations of CrA cluster (Lindberg+, 2012)
J/ApJS/194/43 : YSOs candidates and knots in CrA cloud (Peterson+, 2011)
Byte-by-byte Description of file: stars.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Source name
17- 18 I2 h RAh Right ascension (J2000)
20- 21 I2 min RAm Right ascension (J2000)
23- 27 F5.2 s RAs Right ascension (J2000)
29 A1 --- DE- Declination sign (J2000)
30- 31 I2 deg DEd Declination (J2000)
33- 34 I2 arcmin DEm Declination (J2000)
36- 39 F4.1 arcsec DEs Declination (J2000)
41- 45 F5.2 mag AV ? Extinction
47 A1 --- n_AV [f] f : extinction from SED fitting
49- 53 A5 --- r_AV Reference for extinction, in refs.dat file
55- 77 A23 --- SName Simbad name
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Source name
17 A1 --- n_Name [u] u: for fluxes with large uncertainties (1)
18- 24 F7.2 um lambda Wavelength
27 A1 --- l_Flux Limit flag on Flux
28- 35 E8.3 Jy Flux Flux (2)
36 A1 --- u_Flux Uncertainty flag on Flux
37 A1 --- f_Flux [s] s for potentially saturated photometry
40- 45 E6.2 Jy e_Flux ?=- rms uncertainty on Flux
46- 58 A13 --- r_Flux References, in refs.dat file
60- 72 A13 --- Note Note when combined fluxes (1)
74 A1 --- n_Note [u] u: for fluxes with large uncertainties (1)
--------------------------------------------------------------------------------
Note (1): u: Fluxes with large uncertainties caused by nearby objects or cloud
structures that make it difficult to delimit individual objects
(IRS 7w/e, IRS 5a/b).
Note (2): For G-85, the flux at 1.22um was corrected by the author (the value
in the published paper is a typo).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Ref Reference code
8- 26 A19 --- BibCode BibCode
28- 51 A24 --- Aut Author's name
53- 70 A18 --- Com Comments
--------------------------------------------------------------------------------
History:
From electronic version of the journal
Acknowledgements:
Aurora Sicilia-Aguilar, aurora.sicilia(at)uam.es
(End) Patricia Vannier [CDS] 26-Jun-2013