J/A+A/695/A257 SODA III. binary systems in L1641 and L1647 (Ricciardi+, 2025)
Survey of Orion Disks with ALMA (SODA).
III. Disks in wide binary systems in L1641 and L1647.
Ricciardi G., Van Terwisga S.E., Roccatagliata V., Hacar A., Henning T.,
Del Pozzo W.
<Astron. Astrophys. 695, A257 (2025)>
=2025A&A...695A.257R 2025A&A...695A.257R (SIMBAD/NED BibCode)
ADC_Keywords: Molecular clouds ; Stars, double and multiple ; Stars, masses
Keywords: methods: statistical - protoplanetary disks - binaries: general -
stars: pre-main sequence
Abstract:
Observations of protoplanetary disks within multiple systems in nearby
star-forming regions (SFRs) have shown that the presence of a
neighboring object influences the evolution of dust in disks. However,
the size of the available sample and the separation range covered are
insufficient to fully understand the dust evolution in binary systems.
The goal of this work, based on the Survey of Orion Disks with ALMA
(SODA), is to comprehensively characterize the impact of stellar
multiplicity on Class II disks in the L1641 and L1647 regions of Orion
A (∼1-3Myr). We characterized the protostellar multiplicity using
the Atacama Large Millimeter/submillimeter Array (ALMA), the
ESO-VISTA, and the Hubble Space Telescope. The resulting sample of 65
multiple systems is the largest catalog of wide binary systems to date
(projected separation ≥1000AU) and enables a more robust
statistical characterization of the evolution and properties of
protoplanetary disks.
The disk population was observed in the continuum with ALMA at 225GHz,
with a median rms of 1.5M⊕. We combined these data
(resolution of ∼1.1") with the ESO-VISTA near-infrared survey of the
Orion A cloud (resolution of ∼0.7"). From this dataset, multiple-star
systems were selected using an iterative inside-out search in
projected separation (≥1000AU).
We identify 61 binary systems, 3 triple systems, and 1 quadruple
system. The separation range is between 1000 and 104AU. The dust mass
distributions inferred via the Kaplan-Meier estimator yield a median
mass of 3.23-0.4+0.6M⊕ for primary disks and
3.88-0.3+0.3M⊕ for secondary disks.
Combining our data with those available for the Lupus and Taurus
disks, we identify a threshold separation of about 130AU, beyond
which the previously observed positive correlation between millimeter
flux (and hence dust mass) and projected separation is lost. Recent
theoretical models confirm that pre- and post-threshold systems are
the result of different star formation processes, such as the
fragmentation of gravitationally unstable circumstellar disks, the
thermal fragmentation of infalling cores, or the turbulent
fragmentation of molecular clouds. We can rule out the dependence on
different SFRs: the cumulative mass distributions of multiples in SFRs
of similar ages are statistically indistinguishable. This result
strengthens the hypothesis that there is a universal initial mass
distribution for disks.
Description:
Using the Atacama Large Millimeter/submillimeter Array (ALMA), SODA
(van Terwisga et al., 2022A&A...661A..53V 2022A&A...661A..53V) observed all disks in
these previous Spitzer catalogs located in Orion A below -6 degrees in
declination. The sample of 873 protoplanetary disks was observed with
ALMA at 225GHz, with a median rms of 1.5M⊕ (or 0.08mJy/beam) -
assuming Tdust=20K and kv=2.3cm2/g - and a typical synthesized beam
full width at half maximum of ∼1.1". Further details can be found in
van Terwisga et al. (2022A&A...661A..53V 2022A&A...661A..53V, Cat. J/A+A/661/A53) (Paper
I).
We took a probabilistic approach to identifying multiple systems since
detailed stellar masses and kinematics cannot be obtained for most of
the sample. The probability that two objects are physically
associated, indicating a true multiple system, decreases with the
square of the distance between them.
Our final catalog counts 61 binary systems, 3 triple systems, and 1
quadruple system, located in the regions L1641 and L1647 of Orion A.
Objects:
----------------------------------------------------------
RA (J2000 DE Designation(s)
----------------------------------------------------------
05 39 00.00 -07 00 00.0 L1641 = LDN 1641
05 42 21.02 -09 58 28.5 L1647 = LDN 1647
----------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tabled1.dat 45 65 Multiple systems in the L1641 and L1647 regions
of Orion A
tabled2.dat 55 25 Stellar masses
--------------------------------------------------------------------------------
See also:
J/AJ/144/192 : Spitzer survey of Orion A and B. I. YSO catalog
(Megeath+, 2012)
J/ApJ/818/59 : IN-SYNC. IV. YSOs in Orion A (Da Rio+, 2016)
J/ApJ/821/52 : NIR survey of Spitzer YSOs in Orion Mol. Cloud
(Kounkel+, 2016)
J/A+A/622/A149 : Vienna survey in Orion. III. (Grossschedl+, 2019)
J/A+A/661/A53 : Survey of Orion disks with ALMA (SODA) (van Terwisga+, 2022)
Byte-by-byte Description of file: tabled1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- System Binary of the multiple system
(Vision Index) (ID1-ID2) (1)
10 A1 --- n_System [b] b when same ID1 and ID2
11 A1 --- --- [-]
12- 15 I4 --- System3 ? Third of the multiple system (Vision Index)
16 A1 --- --- [-]
17- 20 I4 --- System4 ? Forth of the multiple system (Vision Index)
22- 28 F7.2 au Sep Separation
30- 36 F7.3 Msun Mass Mean mass
38- 41 F4.2 Msun e_Mass Mean mass error
43- 45 I3 pc Dist Average Distance
--------------------------------------------------------------------------------
Note (1): For binary systems in the Multiple System column, the first Vision
Index corresponds to primary disk, i.e. the brighter one.
Star numbers are [MGM2012] NNNN in Simbad, from Megeath et al.,
2012AJ....144..192M 2012AJ....144..192M; 2016AJ....151....5M 2016AJ....151....5M, Cat. J/AJ/144/192.
References:
(1) van Terwisga et al. (2022A&A...661A..53V 2022A&A...661A..53V, Cat. J/A+A/661/A53);
(2) Grossschedl et al. (2019A&A..622A.149G, Cat. J/A+A/622/A149);
(3) Kounkel et al. (2016ApJ...821...52K 2016ApJ...821...52K. Cat. J/ApJ/821/52).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tabled2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- System Binary of the multiple system (VISION Index)
11- 15 F5.1 Msun MassDD1 Disk dust mass 1st source (1)
17- 20 F4.2 Msun e_MassDD1 Disk dust mass 1st source error
22- 26 F5.2 Msun MassDD2 Disk dust mass 2nd source (1)
28- 31 F4.2 Msun e_MassDD2 Disk dust mass 2nd source error
33- 37 F5.3 Msun MassS1 ?=- Stellar mass 1st source (2)
39- 43 F5.3 Msun e_MassS1 ? Stellar mass 1st source error
45- 49 F5.3 Msun MassS2 ?=- Stellar mass 2nd source (2)
51- 55 F5.3 Msun e_MassS2 ? Stellar mass 2nd source error
--------------------------------------------------------------------------------
Note (1): Reference for disk information:
van Terwisga et al. (2022A&A...661A..53V 2022A&A...661A..53V, Cat. J/A+A/661/A53).
Note (2): Reference for stellar information:
Da Rio et al. (2016ApJ...818...59D 2016ApJ...818...59D, Cat. J/ApJ/818/59);
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
van Terwisga et al. , Paper I 2022A&A...661A..53V 2022A&A...661A..53V, Cat. J/A+A/661/A53
van Terwisga & Hacar, Paper II 2023A&A...673L...2V 2023A&A...673L...2V
(End) Patricia Vannier [CDS] 30-Jul-2025