J/A+A/678/A20 New white dwarf-open cluster associations (Prisegen+, 2023)
Uncovering new white dwarf-open cluster associations using Gaia DR3.
Prisegen M., Faltova N.
<Astron. Astrophys., 678, A20 (2023)>
=2023A&A...678A..20P 2023A&A...678A..20P (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Stars, white dwarf ; Optical ; Stars, masses ;
Stars, ages
Keywords: white dwarfs - open clusters and associations: general - catalogs -
surveys
Abstract:
Open clusters (OCs) provide homogeneous samples of white dwarfs (WDs)
with known distances, extinctions, and total ages. The unprecedented
astrometric precision of Gaia allows us to identify many novel OC-WD
pairs. Studying WDs in the context of their parent OCs makes it
possible to determine the properties of WD progenitors and study the
initial-final mass relation (IFMR).
We seek to find potential new WD members of OCs in the solar vicinity.
The analysis of OC members' parallaxes allows us to determine the OC
distances to a high precision, which in turn enables us to calculate
WD masses and cooling ages and to constrain the IFMR.
We searched for new potential WD members of nearby OCs using the
density-based machine learning clustering algorithm HDBSCAN. The
clustering analysis was applied in five astrometric
dimensions-positions in the sky, proper motions and parallaxes, and in
three dimensions where the positional information was not considered
in the clustering analysis. The identified candidate OC WDs were
further filtered using the photometric criteria and properties of
their putative host OCs. The masses and cooling ages of the WDs were
calculated via a photometric method using all available Gaia,
Pan-STARRS, SDSS, and GALEX photometry. The WD progenitor masses were
determined using the ages and metallicities of their host OCs.
Altogether, 63 OC WD candidates were recovered, 27 of which are
already known in the literature. We provide characterization for 36
novel WDs that have significant OC membership probabilities. Six of
them fall into relatively unconstrained sections of the IFMR where the
relation seems to exhibit nonlinear behavior. We were not able to
identify any WDs originating from massive progenitors that would even
remotely approach the widely adopted WD progenitor mass limit of
8M☉; this confirms the paucity of such objects residing in OCs
and hints at a presence of velocity kicks for nascent WDs.
Description:
We have studied the WD content of nearby OCs with a primary focus on
obtaining tighter constraints on the IFMR, which can be derived
semi-empirically by studying the properties of the WDs and their host
OCs. Our search for WDs within OCs relied on the astrometric and
photometric data provided by the Gaia mission in its third data
release. When such WDs are identified, it is possible to obtain a
significantly more precise distance estimate for the WD, which is
based on robust statistics that are in turn based on a large number of
OC member stars rather than a singular noisy parallax measurement of a
single object. A more precise distance obtained in this way translates
to more precise knowledge of the fundamental WD properties, most
importantly its mass and cooling age. This, in combination with the
knowledge of the total age of the OC and its metallicity, can be used
to constrain the lifetime of the progenitor by subtracting the cooling
age from the total OC age, which can be used to infer the initial mass
of the WD progenitor.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 68 77 WDs and WD candidates recovered as OC members
in the clustering analysis
table2.dat 120 27 Literature WDs recovered as OC members in the
clustering analysis
table3.dat 102 36 Novel or previously uncharacterized WDs recovered
as OC members in the clustering analysis
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- --- [Gaia DR3]
10- 28 I19 --- GaiaDR3 Gaia DR3 source_id
30- 41 A12 --- Assoc Associated open cluster
43- 45 F3.1 --- P3D ?=- Membership probability derived in the
3D membership analysis
48- 50 F3.1 --- P5D ?=- Membership probability derived in the
5D membership analysis
53- 55 F3.1 --- PHR ?=- Membership probability derived in the
Hunt & Reffert (2023A&A...673A.114H 2023A&A...673A.114H,
Cat. J/A+A/673/A114) membership analysis
58- 61 F4.2 --- Fid Astrometric fidelity flag from Rybizki et al.
(2022MNRAS.510.2597R 2022MNRAS.510.2597R)
63- 65 F3.1 --- PWD ?=- Probability of the object being a WD from
Gentile Fusillo et al.
(2021MNRAS.508.3877G 2021MNRAS.508.3877G, Cat. J/MNRAS/508/3877)
68 A1 --- DBM [Y] Y if the object is present as a
spectroscopically confirmed WD in the
Montreal White Dwarf Database
(Dufour et al., 2017, ASP Conf. Ser., 509, 3,
https://www.montrealwhitedwarfdatabase.org)
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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- 19 I19 --- GaiaDR3 Gaia DR3 source_id
21- 32 A12 --- Assoc Associated open cluster
34- 38 F5.3 Msun MWD WD mass
40- 44 F5.3 Msun E_MWD WD mass error (upper value)
46- 50 F5.3 Msun e_MWD WD mass error (lower value)
52- 55 F4.2 Msun Mi Progenitor mass
57- 60 F4.2 Msun E_Mi Progenitor mass error (upper value)
62- 65 F4.2 Msun e_Mi Progenitor mass error (lower value)
67-120 A54 --- Ref Reference for WD and progenitor masses
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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- 19 I19 --- GaiaDR3 Gaia DR3 source_id
21 A1 --- n_GaiaDR3 [a-d] Note on GaiaDR3 (1)
24- 35 A12 --- Assoc Associated open cluster
37- 39 F3.1 --- Pmax Maximum value of astrometric membership
probability from P3D, P5D, and PHR
41- 61 A21 --- APHOT Available photometry
63- 66 F4.2 Msun MWD WD mass (2)
68- 71 F4.2 Msun E_MWD WD mass error (upper value)
73- 76 F4.2 Msun e_MWD WD mass error (lower value)
78- 80 I3 Myr tcool Cooling age (2)
82- 84 I3 Myr E_tcool Cooling age error (upper value)
86- 87 I2 Myr e_tcool Cooling age error (lower value)
89- 92 F4.2 Msun Mi Progenitor mass (2)
94- 97 F4.2 Msun E_Mi Progenitor mass error (upper value)
99-102 F4.2 Msun e_Mi Progenitor mass error (lower value)
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Note (1): Notes as follows:
a = Mentioned in Richer et al. (2021ApJ...912..165R 2021ApJ...912..165R, Cat. J/ApJ/912/165)
but no Mi calculated
b = possible double degenerate system (Williams et al., 2015AJ....150..194W 2015AJ....150..194W)
c = radial velocity possibly inconsistent with OC membership
(Williams et al., 2015AJ....150..194W 2015AJ....150..194W)
d = approximate parameters derived also in Prisegen et al.
(2021A&A...645A..13P 2021A&A...645A..13P) using the GDR2 data
Note (2): WD masses (MWD), cooling ages (tcool), and progenitor masses (Mi)
have been calculated in Sect. 4.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Jan-2024