J/MNRAS/488/1462 New 1.1mm data of IC 348 circumstellar discs (Petersen+, 2019)
Early science with the Large Millimetre Telescope:
new mm-wave detections of circumstellar discs in IC 348 from LMT/AzTEC.
Petersen M.S., Gutermuth R.A., Nagel E., Wilson G.W., Lane J.
<Mon. Not. R. Astron. Soc., 488, 1462-1480 (2019)>
=2019MNRAS.488.1462P 2019MNRAS.488.1462P (SIMBAD/NED BibCode)
ADC_Keywords: YSOs ; Millimetric/submm sources ; Positional data ;
Effective temperatures
Keywords: planets and satellites: individual: protoplanetary discs -
stars: protostars - stars: rotation
Abstract:
We present the most complete sample of mm measurements of
protoplanetary discs in the star-forming region IC 348 to date. New
observations from the Large Millimetre Telescope and the 1.1mm camera
AzTEC are combined with literature results in order to characterize
the disc population as relating to both stellar properties within the
IC 348 region and across other star-forming regions. In addition to
detecting 28 of 116 observed known infrared-excess sources, we
detected emission from two previously unknown candidate transition
discs in the region. When combined with literature results, we find
evidence for a steeper-than-expected slope, on average, in disc
spectral energy distributions at millimetre wavelengths in the IC 348
region. We show that the presence or absence of high-mass discs is a
sensitive indicator of regional evolution, both among star-forming
regions and within IC 348. In contrast, low-mass discs exhibit almost
no apparent evolution within the first ∼5Myr when compared among
regions.
Description:
Our AzTEC observations are centred on known mid-IR-excess-bearing YSO
targets in IC 348 from Gutermuth et al. (2009ApJS..184...18G 2009ApJS..184...18G, Cat.
J/ApJS/184/18).
The data were collected using the 144-element 1.1mm bolometer array
AzTEC (Wilson et al. 2008MNRAS.386..807W 2008MNRAS.386..807W) on the 50-m diameter LMT
during its early science phase when it was limited to a 32-m diameter
collecting area. The LMT observatory employs a dynamic queue strategy
to maximize the use of AzTEC during the best observing conditions.
Using the YSO list of Gutermuth et al. (2009ApJS..184...18G 2009ApJS..184...18G, Cat.
J/ApJS/184/18), we found that 116 total source positions had been
covered, of the complete sample of 160 in Gutermuth et al.
(2009ApJS..184...18G 2009ApJS..184...18G, Cat. J/ApJS/184/18). We extracted sources where
possible, and measured upper limits at the expected source position
for those not detected. We detected 28 sources, with 88 additional
upper limits. Seven sources were detected in multiple fields that had
serendipitous overlapping coverage. 15 additional sources were
detected once and had an additional upper limit in coverage from
another map. The data are given in Table 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 64 116 IR excess matched sources
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See also:
J/ApJS/184/18 : Spitzer survey of young stellar clusters (Gutermuth+, 2009)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- G09 [4/159] YSO identifier from Gutermuth et al.
(2009ApJS..184...18G 2009ApJS..184...18G, Cat. J/ApJS/184/18)
5- 12 F8.5 deg RAdeg Right ascension (J2000) (1)
14- 21 F8.5 deg DEdeg Declination (J2000) (1)
23- 26 F4.1 arcsec dRA Positional offset in right ascension
28- 31 F4.1 arcsec dDE Positional offset in declination
33- 37 F5.2 mJy Flux AzTEC Flux at 1.1mm
39 A1 --- f_Flux Flag on Flux (2)
41- 45 F5.2 --- S/N ?=-1 Signal to noise ratio
47- 53 F7.2 K Teff ?=-1 Effective temperature
55- 60 F6.2 K e_Teff ?=-1 Error on Teff
62- 64 A3 --- Class Source classification (3)
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Note (1): Coordinates are from Gutermuth et al. (2009ApJS..184...18G 2009ApJS..184...18G,
Cat. J/ApJS/184/18)
Note (2): Flag as follows:
* = Potentially contains flux from nearby cloud material
Note (3): Classification as follows:
I = Protostar with an infalling envelope
I* = Deeply embedded source
II = Pre-main sequence star with an optically thick disk
II* = Transition disk candidate
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 01-Dec-2022