J/ApJ/896/81 HST survey of ONC in H2O 1.4um abs. band. III. (Strampelli+, 2020)
HST survey of the Orion Nebula Cluster in the H2O 1.4um absorption band.
III. The population of substellar binary companions.
Strampelli G.M., Aguilar J., Pueyo L., Aparicio A., Gennaro M., Ubeda L.,
Robberto M.
<Astrophys. J., 896, 81 (2020)>
=2020ApJ...896...81S 2020ApJ...896...81S
ADC_Keywords: Stars, double and multiple; Photometry, infrared; Colors;
Stars, masses
Keywords: Binary stars ; Star forming regions ; Low mass stars ;
Substellar companion stars ; Companion stars ; Multiple stars ;
Brown dwarfs ; M dwarf stars
Abstract:
We present new results concerning the substellar binary population in
the Orion Nebula Cluster (ONC). Using the Karhunen-Loeve Image
Projection algorithm, we have reprocessed images taken with the IR
channel of the Wide Field Camera 3 mounted on the Hubble Space
Telescope to unveil faint, close companions in the wings of the
stellar point-spread functions. Starting with a sample of 1392 bona
fide unsaturated cluster members, we detect 39 close-pair cluster
candidates with separation 0.16"-0.77". The primary masses span a
range Mp∼0.015-1.27M☉, whereas for the companions we derive
Mc∼0.004-0.54M☉. Of these 39 binary systems, 18 were already
known, while the remaining 21 are new detections. Correcting for
completeness and combining our catalog with previously detected ONC
binaries, we obtain an overall binary fraction of 11.5%±0.9%.
Compared to other star-forming regions, our multiplicity function is
∼2 times smaller than, for example, Taurus, while compared to the
binaries in the field we obtain comparable values. We analyze the mass
functions of the binaries, finding differences between the mass
distributions of binaries and single stars and between primary and
companion mass distributions. The mass ratio shows a bottom-heavy
distribution with median value Mc/Mp∼0.25. Overall, our results
suggest that ONC binaries may represent a template for the typical
population of field binaries, supporting the hypothesis that the ONC
may be regarded as a most typical star-forming region in the Milky Way.
Description:
We reprocess the full data set of the Cycle 22 HST Treasury Program
"The Orion Nebula Cluster as a Paradigm of Star Formation" (GO-13826,
P.I. M. Robberto; Paper I (Robberto+, 2020, J/ApJ/896/79)) with
advanced PSF subtraction techniques, namely the Karhunen-Loeve
Image Projection (KLIP) algorithm (Soummer+ 2012ApJ...755L..28S 2012ApJ...755L..28S).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 175 39 *Candidate Binaries catalog (KLIP)
table2.dat 175 58 Candidate Binaries catalog (Paper I;
Robberto+, 2020, J/ApJ/896/79)
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Note on table1.dat:
KLIP=the Karhunen-Loeve Image Projection (KLIP) algorithm
(Soummer+ 2012ApJ...755L..28S 2012ApJ...755L..28S); see the Description section.
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See also:
J/A+A/337/403 : Low-mass stars evolutionary models (Baraffe+ 1998)
J/AJ/134/2272 : Visual binaries in the Orion Nebula Cluster (Reipurth+, 2007)
J/ApJ/731/8 : Multiple star formation in Taurus-Auriga (Kraus+, 2011)
J/ApJ/748/14 : ONC population data from WFI observations (Da Rio+, 2012)
J/ApJ/753/156 : T/Y brown dwarfs with WISE photometry (Kirkpatrick+, 2012)
J/ApJS/207/10 : HST Treasury Program on the ONC (Robberto+, 2013)
J/ApJ/794/159 : Statistical analysis of exoplanet surveys (Brandt+, 2014)
J/A+A/627/A57 : ONC binary and triple stars (Jerabkova+, 2019)
J/ApJ/870/32 : Kinematics in young star clusters & associations (Kuhn+, 2019)
J/AJ/157/216 : Multiplicity rate of M dwarfs within 25 pc (Winters+, 2019)
J/ApJ/896/79 : HST survey of ONC in H20 1.4um abs. band. I. (Robberto+, 2020)
Byte-by-byte Description of file: table[12].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Seq [0/96] Catalog entry number
4- 7 I4 --- WFC3IDp [56/4307] Primary ID from Catalog I
(Robberto+, 2020, J/ApJ/896/79)
9- 12 I4 --- WFC3IDc [-1/4308] Companion ID from Catalog I (1)
14- 24 A11 --- Name Simbad name designation
26- 36 F11.8 deg RAdeg [83.6/84] Primary Right Ascension (J2000)
38- 49 F12.9 deg DEdeg [-5.7/-5.2] Primary Declination (J2000)
51- 57 F7.4 mag m130p [11/16.81] Primary F130N filter magnitude
from Catalog I
59- 66 F8.5 mag colorp [-0.41/0.27] Primary F130N-F139M color from
Catalog I
68- 74 F7.5 mag e_m130p [0.0007/0.4] Uncertainty in m130p
76- 82 F7.5 mag e_colorp [9e-5/0.1] Uncertainty in colorp
84- 91 F8.5 mag m130c [11.16/20.1] Companion F130N filter
magnitude from aperture photometry
93-100 F8.5 mag colorc [-0.8/0.35] Companion F130N-F139M color
from aperture photometry
102-108 F7.5 mag e_m130c [0.0007/0.8] Uncertainty in m130c
110-116 F7.5 mag e_colorc [0.0003/0.3] Uncertainty in colorc
118-125 F8.6 Msun Massp [0.01/1.3] Primary mass
127-134 F8.6 Msun Massc [0.004/1.1] Companion mass
136-143 F8.6 Msun e_Massp [3.5e-5/0.4] Error in Massp
145-152 F8.6 Msun e_Massc [3e-5/0.5] Error in Massc
154-159 F6.2 deg PA [6/360] Position angle
161-164 F4.2 arcsec Sep [0.16/1.8] Separation between primary and
companion
166-175 F10.5 arcsec SepOriC [14.6/1065] Distance from teta1 OriC
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Note (1): -1 if the companion is detected through KLIP
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History:
From electronic version of the journal
References:
Strampelli et al. Paper I. 2020ApJ...896...79S 2020ApJ...896...79S Cat. J/ApJ/896/79
Gennaro et al. Paper II. 2020ApJ...896...80G 2020ApJ...896...80G
Strampelli et al. Paper III. 2020ApJ...896...81S 2020ApJ...896...81S This catalog
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 28-Oct-2021