J/A+A/700/A235 CAMPOS II. protostellar disk substructures (Hsieh+, 2025)
CAMPOS II. The onset of protostellar disk substructures and planet formation.
Hsieh C.-H., Arce H.G., Maureira M.J., Pineda J.E., Segura-Cox D.,
Mardones D., Dunham M.M., Li H., Offner S.S.R.
<Astron. Astrophys. 700, A235 (2025)>
=2025A&A...700A.235H 2025A&A...700A.235H (SIMBAD/NED BibCode)
ADC_Keywords: YSOs ; Millimetric/submm sources ; Effective temperatures
Keywords: methods: observational - techniques: interferometric -
planet-disk interactions - stars: low-mass
Abstract:
The 1.3mm CAMPOS survey has resolved 90 protostellar disks with ∼15
au resolution across the Ophiuchus, Corona Australis, and Chamaeleon
star-forming regions. To address the fundamental question, 'When does
planet formation begins, we combined the CAMPOS sample with
literature observations of Class 0-II disks (bolometric temperature,
Tbol≤1900K), all mapped at 1.3mm with resolutions ranging from 4
to 33au. To investigate substructure detection rates as a function of
bolometric temperature, we restricted the sample to disks observed at
the 1.3mm wavelength, with inclinations below 75 degrees, linear
resolution ≤20au and resolved with at least four resolution elements
(θdistk/θres?=4). We also considered the effects of
extinction correction and the inclusion of Herschel Space Telescope
data on the bolometric temperature measurements to constrain the lower
and upper limits of bolometric temperature for each source. We find
that by Tbol∼200-400K, substructure detection rates increased
sharply to ∼60%, corresponding to an approximate age of 0.2-0.4Myr. No
substructures are detected in Class 0 disks. The ratio of
disk-averaged brightness temperature to predicted dust temperature
shows a trend of increasing values toward the youngest Class 0 disks,
suggesting higher optical depths in these early stages. Our
statistical analysis confirms that substructures similar to those in
Class II disks are already common by the Class I stage, and the
emergence of these structures at Tbol∼200-400K could represent only
an upper limit. Classifying disks with substructures into those with
and without large central cavities, we find both populations
coexisting across evolutionary stages, suggesting they are not
necessarily evolutionarily linked. If protostellar disk substructures
do follow an evolutionary sequence, then our results imply that disk
substructures evolve very rapidly and thus can be present in all Class
I/II stages and/or that they can be triggered at different times.
Description:
Class 0/I Protostellar Disks complied from the CAMPOS survey (Hsieh et
al., 2024ApJ...973..138H 2024ApJ...973..138H) (90 disks in Ophiuchus, Corona Australis,
and Chamaeleon), ODISEA survey (Cieza et al., 2019MNRAS.482..698C 2019MNRAS.482..698C,
Cat. J/MNRAS/482/698, 2021MNRAS.501.2934C 2021MNRAS.501.2934C),eDisk survey (Ohashi et
al., 2023ApJ...951....8O 2023ApJ...951....8O), DSHARP survey (Andrews et al.,
2018ApJ...869L..41A 2018ApJ...869L..41A, Cat. J/ApJ/869/L41), and HL Tauri (ALMA
Partnership, 2015ApJ...808L...3A 2015ApJ...808L...3A). Source RA, DEC can be found in the
above survey.
In Table A.2, we cross matched the sources in Corona Australis,
Chamaeleon I & II, Ophiuchus North, and Ophiuchus sources in our
CAMPOS survey with SSTgbs/SSTc2d survey, eHOPS survey, ISO, and IRAS
catalog.
In Table A.3, we cross matched the ODISEA survey with eHOPS and
SSTgbs/SSTc2d. SSTgbs/SSTc2d Names: Spitzer Space Telescope Gould Belt
Survey / Space Telescope core to disk Survey Names. See Dunham et al.
(2015ApJS..220...11D 2015ApJS..220...11D, Cat. J/ApJS/220/11) for the spectral energy
distribution (SED) fitting and the bolometric temperature, and the
bolometric luminosity of the source.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 151 116 Protostellar Disk substructure table
tablea2.dat 140 90 Cross matching Corona Australis, Chamaeleon
I & II, Ophiuchus North, and Ophiuchus sources
in our CAMPOS survey
tablea3.dat 75 53 Cross Matching ODISEA Survey with eHOPS and
SSTgbs/SSTc2d
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See also:
J/MNRAS/482/698 : Ophiuchus DIsc Survey Employing ALMA (ODISEA). I.
(Cieza+, 2019)
J/ApJS/266/32 : Extension of HOPS out to 500pc (eHOPS). I. Aquila
(Pokhrel+, 2023)
https://irsa.ipac.caltech.edu/data/Herschel/eHOPS/overview.html :
eHOPS catalogue
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 22 A22 --- Name Source Name
23 A1 --- n_Name [+cef] Note on Name (1)
25- 30 A6 --- Class Protostellar Class
31 A1 --- n_Class [bd] Note on Class (1)
33- 36 I4 K Tbol Bolometric temperature from eHOPS survey (2)
37 A1 --- n_Tbol [a] Note on Tbol (1)
42- 45 I4 K TbolD Bolometric temperature from Dunham et al.,
2015ApJS..220...11D 2015ApJS..220...11D, Cat. J/ApJS/220/11 (3)
47- 53 F7.4 Lsun Lbol Bolometric luminosity
55- 60 F6.2 10-5Msun Mass Disk dust mass
62- 66 F5.1 au R90 Radius of the disk containing 90% of flux
68- 70 I3 pc Dist Distance to the source
72- 77 F6.1 mJy F1.3mm Total disk continuum flux at 1.3mm
(ALMA Band 6)
79- 80 A2 --- Type Type of substructure (4)
82- 84 I3 mas Beam1 Beam size
85 A1 --- --- [x]
86- 88 I3 mas Beam2 Beam size
91- 94 F4.1 au Res Linear Resolution of the observation
96-100 F5.1 K TbrP Brightness temperature from full Planck
equation
102-106 F5.1 K Tdust Dust temperature of the disk adopting equation
108-119 A12 --- Ref References (For RA, Dec see references) (5)
121-151 A31 --- Cloud Molecular Cloud identifier
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Note (1): Notes as follows:
+ = CFHTWIR-Oph 79 is also known as GY 263 or SKS 3-48 (Wilking et al.,
2015ApJS..220...11D 2015ApJS..220...11D, cat. J/ApJS/220/11; Narayanan et al.,
2023ApJ...958...20N 2023ApJ...958...20N). The classification of this source has been debated.
Narayanan et al. (2023ApJ...958...20N 2023ApJ...958...20N) and Allen et al.
(2002ApJ...566..993A 2002ApJ...566..993A, Cat. J/ApJ/566/993) classified this source as a
Class II disk, while Wilking et al. (2015ApJS..220...11D 2015ApJS..220...11D,
Cat. J/ApJS/220/11) classified it as a Flat spectrum disk based on J, H,
and K band. The source is close to a Class I binary system,
Oph-emb 14 VLA 1&2. In the CAMPOS survey, we assume the same bolometric
temperature and class for all sources in the close multiple systems.
a = In this paper, if the source has no corresponding eHOPS match, we adopt
the non-extinction corrected bolometric temperature from Dunham et al.
(2015ApJS..220...11D 2015ApJS..220...11D, Cat. J/ApJS/220/11).
b = The SED and protostellar system properties are available in
https://irsa.ipac.caltech.edu/data/Herschel/eHOPS/overview.html
(NASA/IPAC Infrared Science Archive). eHOPS classified the source as
Class I, but given its bolometric temperature, it should be Class 0.
c = eHOPS photometry for this source is not centered at the coordinates of
the source for the IRAS 1um image. This could result in the incorrect
value of T_bol. We assigned values from Dunham et al.
(2015ApJS..220...11D 2015ApJS..220...11D, Cat. J/ApJS/220/11).
d = The eHOPS group calculated the spectral index between Spitzer/IRAC 4.5um
and Spitzer/IRAC 24um, and follows Greene et al. (1994ApJ...434..614G 1994ApJ...434..614G)
for Class classification (Pokhrel et al., 2023ApJS..266...32P 2023ApJS..266...32P, Cat.
J/ApJS/266/32). ODISEA C4 081 or eHOPS-oph-22 shows a negative slope
between these wavelengths, resembling a Class II by definition. However,
the source also shows significant emission at longer wavelengths,
resulting in a lower bolometric temperature.
e = eHOPS photometry for this source is not centered at the coordinates of the
source for the IRAS 1-4um image. This could result in the incorrect
value of T_bol. We assigned values from Dunham et al. (2015).
f = eHOPS group updated the SED fit for this source recently, the original
values published in Hsieh et al. (2024ApJ...973..138H 2024ApJ...973..138H) for this source
were outdated.
Note (2): Bolometric temperature from eHOPS catalog. The bolometric temperature
is derived from SED fitting with Herschel Space Telescope longer wavelength
data, but the IR extinction correction is not applied.
Note (3): The bolometric temperature is derived from SED fitting without
Herschel Space Telescope data, but the IR extinction correction is applied.
Note (4): Type of the disk substructure as follows:
NA = no disk substructure is detected
C = a ring with a large central cavity
F = the disk is centrally filled
Note (5): References as follows:
1 = Sources observed in our CAMPOS survey. See also the CAMPOS data paper,
Hsieh et al. (2024ApJ...973..138H 2024ApJ...973..138H), for source identification and
radius measurements.
2 = Murillo et al. (2013A&A...560A.103M 2013A&A...560A.103M)
3 = Hsieh et al. (2020ApJ...894...23H 2020ApJ...894...23H)
4 = Maureira et al. (2022ApJ...941L..23M 2022ApJ...941L..23M)
5 = Ohashi et al. (2023ApJ...951....8O 2023ApJ...951....8O)
6 = Narayanan et al. (2023ApJ...958...20N 2023ApJ...958...20N)
7 = Cieza et al. (2019MNRAS.482..698C 2019MNRAS.482..698C, Cat. J/MNRAS/482/698)
8 = Cieza et al. (2021MNRAS.501.2934C 2021MNRAS.501.2934C)
9 = Segura-Cox et al. (2020Natur.586..228S 2020Natur.586..228S)
10 = Andrews et al. (2018ApJ...869L..41A 2018ApJ...869L..41A, Cat. J/ApJ/869/L41)
11 = Huang et al. (2018ApJ...869L..42H 2018ApJ...869L..42H, Cat. J/ApJ/869/L42)
12 = ALMA Partnership et al. (2015ApJ...808L...3A 2015ApJ...808L...3A)
13 = Wu et al. (2023ApJ...954..190X 2023ApJ...954..190X)
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Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 29 A29 --- Name Name of the source
31- 41 A11 --- CAMPOS CAMPOS ID (1)
43- 65 A23 --- SSTgbs/SSTc2d SSTgbs/SSTc2d Names (2)
67- 79 A13 --- eHOPS eHOPS Name (3)
81- 92 A12 --- ISO Infrared Space Observatory Name (4)
94-108 A15 --- IRAS Infrared Astronomical Satellite Name (5)
110-140 A31 --- Cloud Molecular Cloud identifier
--------------------------------------------------------------------------------
Note (1): CAMPOS ID: Sources observed in our CAMPOS survey. See also the
CAMPOS data paper Hsieh et al. (2024ApJ...973..138H 2024ApJ...973..138H).
Note (2): SSTgbs/SSTc2d Names: Spitzer Space Telescope Gould Belt Survey
/ Space Telescope core to disk Survey Names. See Dunham et al.
(2015ApJS..220...11D 2015ApJS..220...11D, Cat. J/ApJS/220/11) for the spectral energy distribution
(SED) fitting and the bolometric temperature, and the bolometric luminosity of
the source.
Note (3): Extension of HOPS Out to 500 ParSecs (eHOPS) catalog, represents the
latest and most reliable SED fitting to date. The eHOPS catalog contains
1-850um SEDs assembled from 2MASS, Spitzer, Herschel, WISE, and JCMT/SCUBA-2
data. The first paper of eHOPS for Serpens and Aquila molecular clouds was
published by Pokhrel et al. (2023ApJS..266...32P 2023ApJS..266...32P, Cat. J/ApJS/266/32).
For all other clouds, the SED and protostellar system properties are available
in https://irsa.ipac.caltech.edu/data/Herschel/eHOPS/overview.html NASA/IPAC
Infrared Science Archive.
Note (4): Infrared Space Observatory (ISO) source name.
Note (5): Infrared Astronomical Satellite (IRAS) source name.
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Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 --- ODISEA ODISEA source ID, ODISEA C4 NNN
15- 30 A16 --- SSTgbs/SSTc2d SSTgbs/SSTc2d Names
32- 46 A15 --- Name eHOPS Name (1)
48- 62 A15 --- Other Other Name (2)
64 A1 --- Included? [Y/N] Included in the paper (Yes/No)
66- 75 A10 --- Note Other Notes
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Note (1): Extension of HOPS Out to 500 ParSecs (eHOPS), is the latest, most
reliable SED fitting to date. The eHOPS catalog contains 1-850um SEDs assembled
from 2MASS, Spitzer, Herschel, WISE, and JCMT/SCUBA-2 data. The first paper of
eHOPS for Serpens and Aquila molecular clouds was published by Pokhrel et al.
(2023ApJS..266...32P 2023ApJS..266...32P, Cat. J/ApJS/266/32). For all other clouds, the SED and
protostellar system properties are available in
https://irsa.ipac.caltech.edu/data/Herschel/eHOPS/overview.html NASA/IPAC
Infrared Science Archive.
Note (2): Names shown in Table A.1, other higher resolution data available.
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Acknowledgements:
Cheng-Han Hsieh, chenghan.hsieh(at)utexas.edu
References:
Hsieh et al., Paper I 2024ApJ...973..138H 2024ApJ...973..138H
(End) Patricia Vannier [CDS] 29-Jun-2025