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J/ApJ/707/1836              BLAST survey in Vela-D                 (Olmi+, 2009)

The BLAST survey of the Vela molecular cloud: physical properties of the dense cores in Vela-D. Olmi L., Ade P.A.R., Angles-Alcazar D., Bock J.J., Chapin E.L., De Luca M., Devlin M.J., Dicker S., Elia D., Fazio G.G., Giannini T., Griffin M., Gundersen J.O., Halpern M., Hargrave P.C., Hughes D.H., Klein J., Lorenzetti D., Marengo M., Marsden G., Martin P.G., Massi F., Mauskopf P., Netterfield C.B., Patanchon G., Rex M., Salama A., Scott D., Semisch C., Smith H.A., Strafella F., Thomas N., Truch M.D.P., Tucker C., Tucker G.S., Viero M.P., Wiebe D.V. <Astrophys. J., 707, 1836-1851 (2009)> =2009ApJ...707.1836O
ADC_Keywords: Photometry, millimetric/submm ; Photometry, infrared ; Surveys ; Molecular clouds Keywords: balloons - ISM: clouds - stars: formation - submillimeter Abstract: The Balloon-borne Large-Aperture Submillimeter Telescope (BLAST) carried out a 250, 350, and 500um survey of the Galactic plane encompassing the Vela Molecular Ridge, with the primary goal of identifying the coldest dense cores possibly associated with the earliest stages of star formation. Here, we present the results from observations of the Vela-D region, covering about 4deg2, in which we find 141 BLAST cores. We exploit existing data taken with the Spitzer MIPS, IRAC, and SEST-SIMBA instruments to constrain their (single-temperature) spectral energy distributions, assuming a dust emissivity index β=2.0. This combination of data allows us to determine the temperature, luminosity, and mass of each BLAST core, and also enables us to separate starless from protostellar sources. We also analyze the effects that the uncertainties on the derived physical parameters of the individual sources have on the overall physical properties of starless and protostellar cores, and we find that there appear to be a smooth transition from the pre- to the protostellar phase. In particular, for protostellar cores we find a correlation between the MIPS24 flux, associated with the central protostar, and the temperature of the dust envelope. We also find that the core mass function of the Vela-D cores has a slope consistent with other similar (sub)millimeter surveys. Description: In this paper, we use both BLAST (2006 science flight; 1.8m Cassegrain telescope with FWHM of 36", 42", and 60" at 250, 350, and 500um) and archival data (SEST/SIMBA, Spitzer/MIPS & IRAC, Akari/FIS) to determine the SEDs, and thus physical parameters, of each source detected by BLAST. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 124 141 BLAST sources table2.dat 75 141 1.2mm-24 micron counterparts
See also: II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986) J/ApJ/719/9 : IRAC point-source catalog of Vela-D cloud (Strafella+, 2010) J/ApJ/704/606 : Protostars in the Vela Molecular Cloud (Giannini+, 2009) J/ApJ/707/1824 : Cold cores in Vela (Netterfield+, 2009) J/ApJ/681/428 : BLAST sources in Galactic plane survey (Chapin+, 2008) J/ApJ/671/470 : MIPS survey of YSOs in Vela Molecular Ridge-D (Giannini+, 2007) J/A+AS/136/471 : JHK photometry of D-cloud IRAS sources (Massi+, 1999) http://www.sciops.esa.int/index.php?project=ASTROF&page=observers : Akari observers page Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [0,140] Running source identification number 5- 9 A5 --- --- [BLAST] 11- 24 A14 --- BLAST Source name (JHHMMSS+DDMMSS) 26- 33 F8.4 deg GLON Galactic longitude 35- 41 F7.4 deg GLAT Galactic latitude 43- 47 F5.1 Jy S250 BLAST flux density at 250um (1) 49- 52 F4.1 Jy e_S250 Uncertainty in S250 (2) 54- 58 F5.1 Jy S350 BLAST flux density at 350um (1) 60- 63 F4.1 Jy e_S350 Uncertainty in S350 (2) 65- 69 F5.1 Jy S500 BLAST flux density at 500um (1) 71- 74 F4.1 Jy e_S500 Uncertainty in S500 (2) 76- 79 F4.1 K T Source temperature (1) 81- 84 F4.1 K E_T Upper limit uncertainty in T (2) 86- 88 F3.1 K e_T Lower limit uncertainty in T (2) 90- 93 F4.1 Msun Mass Source mass (1) 95- 98 F4.1 Msun E_Mass Upper limit uncertainty in Mass (2) 100-103 F4.1 Msun e_Mass Lower limit uncertainty in Mass (2) 105-109 F5.1 Lsun Lum Source luminosity (1) 111-114 F4.1 Lsun E_Lum Upper limit uncertainty in Lum (2) 116-119 F4.1 Lsun e_Lum Lower limit uncertainty in Lum (2) 121-124 F4.2 pc Diam Deconvolved diameter (3)
Note (1): Using SED fits to obtain color-corrections for the band-averaged flux densities (Chapin et al. 2008, Cat. J/ApJ/681/428; Truch et al. 2008ApJ...681..415T). Note (2): The quoted statistical uncertainties are determined from Monte Carlo simulations and do not include calibration uncertainties (see Section 4). Note (3): The deconvolved or intrinsic source FWHM is obtained from the best-fit source size, θfit, and the BLAST beam size, θb, as θdec=(θfit2b2)1/2 (Netterfield et al. 2009, Cat. J/ApJ/707/1824).
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [0,140] Running source identification number 5- 9 A5 --- --- [BLAST] 11- 24 A14 --- BLAST Source name (JHHMMSS+DDMMSS) 26- 29 F4.2 Jy S1200 ? SEST/SIMBA flux density at 1200um (4) 31 A1 --- f_S1200 [a] Indicates aperture photometry 33 I1 --- o_S1200 [0,2]? Number of sources at S1200 (5) 35- 40 F6.1 Jy S100 ? IRAS flux density at 100um (4) 42 A1 --- f_S100 [a] Indicates aperture photometry 44- 48 F5.1 Jy S60 ? IRAS flux density at 60um (4) 50 A1 --- f_S60 [a] Indicates aperture photometry 52 I1 --- o_S100 [0/1] Number of IRAS-PSC sources associated with BLAST core (5) 54 I1 --- o_S60 [0,2] Number of Akari sources associated with BLAST core (5) 56- 61 F6.2 Jy S70 ? Spitzer/MIPS flux density at 70um (4) 63 A1 --- f_S70 [a] Indicates aperture photometry 65 I1 --- o_S70 [0,2]? Number of sources at S70 (5) 67- 71 F5.3 Jy S24 ? Spitzer/MIPS flux density at 24um (4) 73 I1 --- o_S24 [0,4]? Number of sources at S24 (5) 75 I1 --- Nmsx [0/1] Number of MSX sources (Cat. V/114) (5)
Note (4): When the number of sources is 0, but the flux density is not zero, then an upper limit to the flux is listed, either estimated by aperture photometry (the "a" flag) or by determining the noise in the map. Note (5): The search radius is a variable function of both BLAST and the ancillary instrument positional uncertainties (see section 3.1).
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 06-Jan-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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