J/MNRAS/478/3674 IC 348 circumstellar discs ALMA data (Ruiz-Rodriguez+, 2018)
ALMA survey of circumstellar discs in the young stellar cluster IC 348.
Ruiz-Rodriguez D., Cieza L.A., Williams J.P., Andrews S.M., Principe D.A.,
Caceres C., Canovas H., Casassus S., Schreiber M.R., Kastner J.H.
<Mon. Not. R. Astron. Soc., 478, 3674-3692 (2018)>
=2018MNRAS.478.3674R 2018MNRAS.478.3674R (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Interferometry ; Infrared sources ;
Stars, masses
Keywords: instrumentation: interferometers - planetary systems
Abstract:
We present a 1.3mm continuum survey of the young (2-3Myr) stellar
cluster IC 348 that lies at a distance of 310pc and is dominated by
low-mass stars (M*∼0.1-0.6M☉). We observed 136 Class II sources
(discs that are optically thick in the infrared) at 0.8arcsec (200au)
resolution with a 3σ sensitivity of ∼0.45mJy
(Mdust∼1.3M⊕). We detect 40 of the targets and construct a
mm-continuum luminosity function. We compare the disc mass
distribution in IC 348 to those of younger and older regions, taking
into account the dependence on stellar mass. We find a clear evolution
in disc masses from 1 to 5-10Myr. The disc masses in IC 348 are
significantly lower than those in Taurus (1-3Myr) and Lupus (1-3Myr),
similar to those of Chamaleon I, (2-3Myr) and σ Ori (3-5Myr) and
significantly higher than in Upper Scorpiusrpius (5-10Myr). About 20
discs in our sample (∼5 percent of the cluster members) have estimated
masses (dust+gas)>1MJup and hence might be the precursors of giant
planets in the cluster. Some of the most massive discs include
transition objects with inner opacity holes based on their infrared
Spectral Energy Distribution (SEDs). From a stacking analysis of the
96 non-detections, we find that these discs have a typical dust mass
of just ≤0.4M⊕, even though the vast majority of their
infrared SEDs remain optically thick and show little signs of
evolution. Such low-mass discs may be the precursors of the small
rocky planets found by Kepler around M-type stars.
Description:
ALMA observations towards our IC 348 targets were carried out in
Band 6 (211-275GHz) under the project code: 2015.1.01037.S. Our
science goal was executed in Cycle 3 with the C40-4 array
configuration and was observed between the 2015 June 23 and 2015 June
27. The Band 6 continuum observations were conducted with a total
on-source integration time of ∼1min per target over three execution
blocks, each one targeting all 136 objects for 0.3min. The adopted
setup included two spectral windows for continuum observations with
effective bandwidths of 1.875GHz centred at 218.0 and 233.0GHz, for a
mean frequency of 225.676GHz (∼1.3mm).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 71 136 Targeted Class II Objects in IC 348
table2.dat 19 96 Non-Detected Class II Sources in IC 348
table3.dat 53 40 Continuum detections of Class II sources in IC 348
table5.dat 62 136 Stellar properties for Class II sources in IC 348
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See also:
J/A+A/409/147 : J magnitude of IC 348 brown dwarfs (Preibisch+, 2003)
J/AJ/131/1574 : Infrared photometry of IC348 members (Lada+, 2006)
J/AJ/134/411 : Properties of IC 348 members (Muench+, 2007)
J/A+A/539/A64 : X-ray data for IC 348 young stars (Alexander+, 2012)
J/AJ/145/66 : Spitzer light curves of YSOs in IC 348 (Flaherty+, 2013)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/136] Source ID
4 A1 --- n_Seq [*] * for transitional disc
6- 31 A26 --- Target Star name
33- 34 I2 h RAh Right ascension (J2000)
36- 37 I2 min RAm Right ascension (J2000)
39- 43 F5.2 s RAs Right ascension (J2000)
45 A1 --- DE- Declination sign (J2000)
46- 47 I2 deg DEd Declination (J2000)
49- 50 I2 arcmin DEm Declination (J2000)
52- 56 F5.2 arcsec DEs Declination (J2000)
58- 66 A9 --- SpType Spectral type
68- 71 A4 --- Ref References (1)
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Note (1): References as follows:
1 = Lada et al. (2006, Cat. J/AJ/131/1574)
2 = Muench et al. (2007, Cat. J/AJ/134/411)
3 = Espaillat et al. (2012ApJ...747..103E 2012ApJ...747..103E)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/136] Source ID
5- 9 F5.2 mJy F1.3mm Flux at 1.3mm
11- 14 F4.2 mJy e_F1.3mm Flux at 1.3mm error
16- 19 F4.2 mJy/beam rms rms
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/136] Source ID
5- 9 F5.2 mJy F1.3mm Integrated flux density a 1.3mm (1)
11- 14 F4.2 mJy e_F1.3mm Integrated flux density a 1.3mm error (1)
16- 19 F4.2 mJy/beam rms rms
21- 25 F5.2 arcsec ORA Right ascension offset from the phase centre (1)
27- 31 F5.2 arcsec ODE Declination offset from the phase centre (1)
33- 36 F4.2 arcsec a ? FWHM along the major axis (1)
38- 41 F4.2 arcsec e_a ? FWHM along the major axis error (1)
43- 48 F6.2 Mgeo Mdust Dust mass
50- 53 F4.2 Mgeo e_Mdust Dust mass error
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Note (1): The elliptical Gaussian model applied to the resolved sources
generates five free parameters.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/136] Source ID
5- 8 F4.2 [K] logTeff ? Effective temperature
10- 13 F4.2 [K] E_logTeff ? Error on logTeff (upper value)
15- 18 F4.2 [K] e_logTeff ? Error on logTeff (lower value)
20- 24 F5.2 mag Av ? Absorption in V band
26- 29 F4.2 mag e_Av ? Absorption in V band error
31- 36 F6.3 [Lsun] logL* ? Luminosity
38- 41 F4.2 [Lsun] E_logL* ? Error on Luminosity (upper value)
43- 46 F4.2 [Lsun] e_logL* ? Error on Luminosity (lower value)
48- 52 F5.3 Msun M* ? Stellar mass
54- 57 F4.2 Msun E_M* ? Error on stellar mass (upper value)
59- 62 F4.2 Msun e_M* ? Error on stellar mass (lower value)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 24-Aug-2021