J/ApJ/890/130 VANDAM survey of Orion protostars. II. (Tobin+, 2020)
The VLA/ALMA Nascent Disk And Multiplicity (VANDAM) survey of Orion protostars.
II. A statistical characterization of class 0 and class I protostellar disks.
Tobin J.J., Sheehan P.D., Megeath S.T., Diaz-Rodriguez A.K., Offner S.S.R.,
Murillo N.M., van 't Hoff M.L.R., van Dishoeck E.F., Osorio M., Anglada G.,
Furlan E., Stutz A.M., Reynolds N., Karnath N., Fischer W.J., Persson M.,
Looney L.W., Li Z.-Y., Stephens I., Chandler C.J., Cox E., Dunham M.M.,
Tychoniec L., Kama M., Kratter K., Kounkel M., Mazur B., Maud L., Patel L.,
Perez L., Sadavoy S.I., Segura-Cox D., Sharma R., Stephenson B.,
Watson D.M., Wyrowski F.
<Astrophys. J., 890, 130 (2020)>
=2020ApJ...890..130T 2020ApJ...890..130T
ADC_Keywords: YSOs ; Photometry, millimetric/submm; Stars, diameters; Surveys
Keywords: Protostars ; Protoplanetary disks ; Young stellar objects ;
Star formation
Abstract:
We have conducted a survey of 328 protostars in the Orion molecular
clouds with the Atacama Large Millimeter/submillimeter Array at 0.87mm
at a resolution of ∼0.1" (40au), including observations with the Very
Large Array at 9mm toward 148 protostars at a resolution of ∼0.08"
(32au). This is the largest multiwavelength survey of protostars at
this resolution by an order of magnitude. We use the dust continuum
emission at 0.87 and 9mm to measure the dust disk radii and masses
toward the Class 0, Class I, and flat-spectrum protostars,
characterizing the evolution of these disk properties in the
protostellar phase. The mean dust disk radii for the Class 0, Class I,
and flat-spectrum protostars are 44.9-3.4+5.8, 37.0-3.0+4.9,
and 28.5-2.3+3.7au, respectively, and the mean protostellar dust
disk masses are 25.9-4.0+7.7, 14.9-2.2+3.8,
11.6-1.9+3.5M⊕, respectively. The decrease in dust disk
masses is expected from disk evolution and accretion, but the decrease
in disk radii may point to the initial conditions of star formation
not leading to the systematic growth of disk radii or that radial
drift is keeping the dust disk sizes small. At least 146 protostellar
disks (35% of 379 detected 0.87mm continuum sources plus 42
nondetections) have disk radii greater than 50au in our sample. These
properties are not found to vary significantly between different
regions within Orion. The protostellar dust disk mass distributions
are systematically larger than those of Class II disks by a factor of
>4, providing evidence that the cores of giant planets may need to at
least begin their formation during the protostellar phase.
Description:
The sample of protostars is drawn from the Herschel Orion Protostar
Survey (HOPS; Fischer+ 2010A&A...518L.122F 2010A&A...518L.122F ; Stutz+ 2013, J/ApJ/767/36
and Furlan+ 2016, J/ApJS/224/5).
ALMA is located in northern Chile on the Chajnantor Plateau at an
elevation of ∼5000m. The protostars in Orion selected for observations
with ALMA at 0.87mm were divided into three scheduling blocks. One
scheduling block contained the selected protostars in the Orion B
molecular cloud, and two other scheduling blocks contained the
selected protostars in the Orion A molecular cloud. Each scheduling
block was successfully executed three times, for nine executions in
total. Six were executed in 2016 September, and three were executed in
2017 July. See Section 2.2.
We conducted observations with the VLA in the A configuration between
2016 October 20 and 2017 January 7 in ∼100 individual observations.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 68 331 ALMA fields
table4.dat 67 109 VLA fields
table6.dat 152 425 ALMA source properties
table7.dat 152 276 VLA source properties
table8.dat 182 476 ALMA and VLA derived parameters
--------------------------------------------------------------------------------
See also:
J/A+A/291/943 : Protostellar cores (Ossenkopf+, 1994)
J/ApJ/675/491 : Lynds 988e JHKs and IRAC photometry (Allen+, 2008)
J/ApJ/686/1195 : IR photometry in the γ Vel cluster (Hernandez+, 2008)
J/ApJ/692/973 : Protostars in Perseus, Serpens and Ophiuchus (Enoch+, 2009)
J/ApJS/181/321 : Properties of Spitzer c2d dark clouds (Evans+, 2009)
J/A+A/494/147 : Young TTau star in CB26 molecular outflows (Launhardt+, 2009)
J/AJ/144/192 : Spitzer survey of Orion A and B. I. YSO cat. (Megeath+, 2012)
J/ApJ/771/129 : Submillimetric Class II sources of Taurus (Andrews+, 2013)
J/ApJ/767/36 : APEX observations of HOPS protostars (Stutz+, 2013)
J/A+A/563/L3 : NGC1333-IRAS2A SiO & SO maps (Codella+, 2014)
J/A+A/566/A45 : Orion optical-depth and column-density maps (Lombardi+, 2014)
J/ApJS/220/11 : SEDs of Spitzer YSOs in the Gould Belt (Dunham+, 2015)
J/ApJ/806/231 : MISFITS survey: HCO+ obs. of Spitzer YSOs (Heiderman+, 2015)
J/ApJ/828/46 : ALMA survey of Lupus protopl. disks. I. (Ansdell+, 2016)
J/ApJ/827/142 : ALMA obs. of GKM stars in Upper Sco (Barenfeld+, 2016)
J/ApJS/224/5 : Herschel Orion Protostar Survey (HOPS): SEDs (Furlan+, 2016)
J/ApJ/831/125 : ALMA 887µm obs. of ChaI (Pascucci+, 2016)
J/A+A/587/A47 : SMA 1.3mm image of OMC 1 North (Teixeira+, 2016)
J/ApJ/834/142 : Gould's Belt Distances Survey. II. OMC (Kounkel+, 2017)
J/ApJ/845/44 : 340GHz SMA obs. of 50 protoplanetary disks (Tripathi+, 2017)
J/A+A/616/A56 : [BHB2007] 11 full stokes continuum ALMA images (Alves+, 2018)
J/ApJ/869/L41 : DSHARP I. Sample, ALMA obs. log and overview (Andrews+, 2018)
J/ApJ/859/21 : ALMA survey of Lupus protopl. disks. II. (Ansdell+, 2018)
J/AJ/156/84 : APOGEE-2 survey of Orion Complex. II. (Kounkel+, 2018)
J/ApJ/865/73 : GOBELINS. V. Kinematics of Perseus (Ortiz-Leon+, 2018)
J/AJ/155/54 : TBOSS Survey. II. ALMA continuum obs. (Ward-Duong+, 2018)
J/A+A/626/A11 : Corona Australis ALMA and X-Shooter data (Cazzoletti+, 2019)
J/MNRAS/482/698 : Oph DIsc Survey Employing ALMA (ODISEA). I. (Cieza+, 2019)
J/ApJ/884/6 : Known members of Orion A with Gaia DR2 data (McBride+, 2019)
J/A+A/628/A85 : Disk masses in Orion Molecular Cloud-2 (van Terwisga+, 2019)
J/ApJ/875/L9 : ODISEA: Disk dust mass distributions (Williams+, 2019)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- FieldA ALMA field name (1)
14 A1 --- n_FieldA [d] d=duplicate fields (2)
16- 17 I2 h RAh [5] Field hour of Right Ascension (J2000)
19- 20 I2 min RAm [33/54] Field minute of Right Ascension (J2000)
22- 27 F6.3 s RAs Field second of Right Ascension (J2000)
29 A1 --- DE- Field sign of the Declination (J2000)
30- 31 I2 deg DEd [0/8] Field degree of Declination (J2000)
33- 34 I2 arcmin DEm Field arcminute of Declination (J2000)
36- 40 F5.2 arcsec DEs Field arcsecond of Declination (J2000)
42- 47 F6.1 Lsun Lbol [0/1478] Bolometric luminosity
49- 54 F6.1 K Tbol [23/1211] Bolometric temperature
56- 61 F6.1 pc Dist [351/441.1] Distance estimate toward protostar
63- 66 A4 --- Class Protostellar class (3)
68 I1 --- Nsrc [0/7] Sources detected per field
--------------------------------------------------------------------------------
Note (1): The field names that begin with S13 are taken from
Stutz+ (2013, J/ApJ/767/36), which identified them as
potential protostellar sources. However, no sources were detected
within the S13 fields.
Note (2): The fields HOPS-395, HOPS-406, and HOPS-408 were target name being
assigned to the same position.
Note (3): Protostellar class as follows:
0 = Class 0 protostar (97 occurrences)
I = Class I protostar (128 occurrences)
Flat = Flat spectrum protostar (103 occurrences)
None = (3 occurrences)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- FieldV VLA field name(s) (1)
14- 15 I2 h RAh [5] Field hour of Right Ascension (J2000)
17- 18 I2 min RAm [33/54] Field minute of Right Ascension (J2000)
20- 25 F6.3 s RAs Field second of Right Ascension (J2000)
27 A1 --- DE- Field sign of the Declination (J2000)
28- 29 I2 deg DEd Field degree of Declination (J2000)
31- 32 I2 arcmin DEm Field arcminute of Declination (J2000)
34- 38 F5.2 arcsec DEs Field arcsecond of Declination (J2000)
40- 45 F6.1 Lsun Lbol [0.1/1478]?=-99 Bolometric luminosity
47- 52 F6.1 K Tbol [23/492]?=-99 Bolometric temperature
54- 59 F6.1 pc Dist [355.4/440.3] Distance estimate toward protostar
61- 64 A4 --- Class Protostellar class (2)
66- 67 I2 --- Nsrc [0/18] Sources detected per field
--------------------------------------------------------------------------------
Note (1): When a field appears twice, the purpose is to list the Lbol, Tbol,
and different distance estimates that may exist when know for the
individual protostars contained within each field.
Note (2): Protostellar class as follows:
0 = Class 0 protostar (85 occurrences)
I = Class I protostar (19 occurrences)
Flat = Flat spectrum protostar (1 occurrence)
None = (4 occurrences)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 25 A25 --- Name Name of source
27- 28 I2 h RAh [5]? Field hour of Right Ascension (J2000)
30- 31 I2 min RAm [33/54]? Field minute of
Right Ascension (J2000)
33- 38 F6.3 s RAs ? Field second of Right Ascension (J2000)
41 A1 --- DE- Field sign of the Declination (J2000)
42- 43 I2 deg DEd ? Field degree of Declination (J2000)
45- 46 I2 arcmin DEm ? Field arcminute of Declination (J2000)
48- 52 F5.2 arcsec DEs ? Field arcsecond of Declination (J2000)
55- 66 A12 --- FieldA ALMA field name
68- 72 F5.1 arcsec DistFA [0/14.6] Source distance
from ALMA phase center
74- 85 A12 --- FieldV VLA field name
87- 91 F5.1 arcsec DistFV [0/57]?=-99 Source distance
from VLA phase center
93- 96 A4 --- Class Protostellar class
98-105 F8.3 mJy Flux [0.9/1587.4]?=-99 Integrated flux density
ALMA 0.87mm
107-114 F8.3 mJy e_Flux [0.19/33.5]?=-99 Uncertainty in Flux
116-123 F8.3 mJy/beam PFlux [0.9/193]?=-99 Peak intensity ALMA 0.87mm
125-130 F6.2 mJy/beam RMS [0.19/5.6] RMS noise in ALMA 0.87mm image
132-137 F6.2 arcsec dBmaj [0/1.6]?=-99 Deconvolved Major Axis
139-144 F6.2 arcsec dBmin [0/0.6]?=-99 Deconvolved Minor Axis
146-150 F5.1 deg dPA [0/179.4]?=-99 Deconvolved Position Angle
152 A1 --- Flag ALMA detection flag (1)
--------------------------------------------------------------------------------
Note (1): ALMA detection flag as follows:
d = detection (380 occurrences)
u = non-detection (45 occurrences)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 25 A25 --- Name Name of source
27- 28 I2 h RAh [5]? Field hour of Right Ascension (J2000)
30- 31 I2 min RAm [33/54]? Field minute of
Right Ascension (J2000)
33- 38 F6.3 s RAs ? Field second of Right Ascension (J2000)
41 A1 --- DE- Field sign of the Declination (J2000)
42- 43 I2 deg DEd ? Field degree of Declination (J2000)
45- 46 I2 arcmin DEm ? Field arcminute of Declination (J2000)
48- 52 F5.2 arcsec DEs ? Field arcsecond of Declination (J2000)
55- 66 A12 --- FieldA ALMA field name
68- 72 F5.1 arcsec DistFA [0/16.5]?=-99 Source distance
from ALMA phase center
74- 85 A12 --- FieldV VLA field name
87- 91 F5.1 arcsec DistFV [0/57] Source distance from VLA phase center
93- 96 A4 --- Class Protostellar class
98-105 F8.3 mJy Flux [0.02/51.4]?=-99 Integrated flux density
VLA 9mm
107-114 F8.3 mJy e_Flux [0/0.2]?=-99 Uncertainty in Flux
116-123 F8.3 mJy/beam PFlux [0.02/24.3]?=-99 Peak intensity VLA 9mm
125-130 F6.2 mJy/beam RMS [5/63.1] RMS noise VLA 9mm
132-137 F6.2 arcsec dBmaj [0/0.4]?=-99 Deconvolved Major Axis
139-144 F6.2 arcsec dBmin [0/0.3]?=-99 Deconvolved Minor Axis
146-150 F5.1 deg dPA [0/173]?=-99 Deconvolved Position Angle
152 A1 --- Flag VLA detection flag (1)
--------------------------------------------------------------------------------
Note (1): VLA detection flag as follows:
d = detection (232 occurrences)
u = non-detection (44 occurrences)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 25 A25 --- Name Name of source
27- 28 I2 h RAh [5]? Field hour of Right Ascension (J2000)
30- 31 I2 min RAm [33/54]? Field minute of
Right Ascension (J2000)
33- 38 F6.3 s RAs ? Field second of Right Ascension (J2000)
41 A1 --- DE- Field sign of the Declination (J2000)
42- 43 I2 deg DEd ? Field degree of Declination (J2000)
45- 46 I2 arcmin DEm ? Field arcminute of Declination (J2000)
48- 52 F5.2 arcsec DEs ? Field arcsecond of Declination (J2000)
54- 59 F6.1 Lsun Lbol [0/1405]?=-99 Bolometric luminosity
61- 66 F6.1 K Tbol [23/1211]?=-99 Bolometric temperature
68- 71 A4 --- Class Protostellar class (1)
73- 77 F5.1 AU RdiskA [7/511.2]?=-99 Disk radius ALMA
79- 83 F5.1 AU e_RdiskA [10/33]?=-99 Uncertainty in RdiskA
85- 89 F5.1 AU RdiskV [2.3/137]?=-99 Disk radius VLA
91- 95 F5.1 AU e_RdiskV [10/29.2]?=-99 Uncertainty in RdiskV
97- 98 A2 --- l_MdiskA [≤ ] Limit flag on MdiskA
100-107 F8.1 Mgeo MdiskA [0.5/1059]?=-99 Disk mass ALMA (2)
109-116 F8.1 Mgeo e_MdiskA [0.1/19]?=-99 Uncertainty in MdiskA
118-119 A2 --- l_MdiskV [≤ ] Limit flag on MdiskV
121-128 F8.1 Mgeo MdiskV [6.3/77023.1]?=-99 Disk mass VLA (2)
130-137 F8.1 Mgeo e_MdiskV [0/111]?=-99 Uncertainty in MdiskV
139-144 F6.2 --- QALMA [0.2/373]?=-99 Toomre Q ALMA (3)
146-151 F6.2 --- QVLA [0.01/14.6]?=-99 Toomre Q VLA (3)
153-158 F6.1 --- SpIdxAV [1/3.2]?=-99 Spectral index 0.87mm to 9mm
160-165 F6.2 --- e_SpIdxAV [0.06/0.2]?=-99 Uncertainty in SpIdxAV
167-172 F6.1 --- SpIdxV [-2.8/12]?=-99 Spectral index 8.1mm to 1cm
174-179 F6.2 --- e_SpIdxV [0/3.8]?=-99 Uncertainty in SpIdxV
181-182 A2 --- Flag Detection flags (4)
--------------------------------------------------------------------------------
Note (1): Protostellar class as follows:
0 = Class 0 protostar (149 occurrences)
I = Class I protostar (150 occurrences)
II = Class II protostar (1 occurrence)
Flat = Flat spectrum protostar (132 occurrence)
None = (44 occurrences)
Note (2): Dust mass calculated assuming Kappa0.87=1.84cm2/g and
Kappa9mm=0.144cm2/g and Tdust=43K*Lbol0.25 and
multiplied by 100 (the gas to dust mass ratio). If Lbol is not known,
0 solar luminosity is assumed.
Note (3): Considering a simplified relationship for Toomre's Q from
Kratter & Lodato (2016ARA&A..54..271K 2016ARA&A..54..271K), we can use the distribution of
dust disk masses to infer which disks are most likely to be unstable
with a few assumptions. Here Q can be approximated as Equation (3):
Q∼2(M*/Md)(H/R) where M* is the mass of the protostar (in solar
masses), Md is the total mass of the disk (gas and dust) in solar
masses, H is the vertical scale height of the disk, and R is the
radius of the disk. A disk is considered gravitationally unstable for
values of Q<1 and marginally unstable for 2.5>Q≥1. See Section 4.4.
Note (4): This string has two characters, the first character refers to
the ALMA data and the second character refers to the VLA data. The
character 'd' refers to a detection, 'u' is a non-detection, and 'n'
is no observations.
An explicit key is provided in the following:
dd = ALMA detection and VLA detection (177 occurrences);
du = ALMA detection and VLA non-detection (35 occurrences);
dn = ALMA detection and no VLA observations (168 occurrences);
ud = ALMA non-detection and VLA detection (4 occurrences);
nd = ALMA no observations and VLA detection (51 occurrences);
uu = ALMA non-detection and VLA non-detection (9 occurrences);
nu = ALMA no observations and VLA non-detection (0 occurrence);
un = ALMA non-detection and no VLA observations (32 occurrences).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Tobin et al. Paper I. 2019ApJ...886....6T 2019ApJ...886....6T
Tobin et al. Paper II. 2020ApJ...890..130T 2020ApJ...890..130T This catalog
Sheehan et al. Paper III. 2020ApJ...902..141S 2020ApJ...902..141S
Tobin et al. Paper IV. 2020ApJ...905..162T 2020ApJ...905..162T
Tobin et al. Paper V. 2022ApJ...925...39T 2022ApJ...925...39T Cat. J/ApJ/925/39
Sheehan et al. Paper VI. 2022ApJ...929...76S 2022ApJ...929...76S Cat. J/ApJ/929/76
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Oct-2021