J/A+A/688/A168 Bright white dwarfs with IR excess (Madurga Favieres+, 2024)
AA sample of 554 white dwarfs showing infrared excess from Gaia EDR3 and
CatWISE catalogs.
Madurga Favieres C., Kissler-Patig M., Xu S., Bonsor A.
<Astron. Astrophys. 688, A168 (2024)>
=2024A&A...688A.168M 2024A&A...688A.168M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, white dwarf ; Infrared sources
Keywords: catalogs - circumstellar matter - infrared: stars
Abstract:
White dwarfs (WDs) are generally intrinsically faint in the infrared
(IR). Excess emission in the infrared results from low-mass companions
or dusty material, potentially linked to the on-going accretion of
planetary material.
This work presents a new catalog of white dwarfs with (candidate)
infrared excess.
The final sample comes from a cross-match between the Gaia Early Data
Release (EDR3) white dwarf candidates, and the CatWISE catalog, with
candidate infrared excesses determined considering both magnitude and
color excess. A magnitude excess is found to be more reliable than a
color excess.
The final catalog contains 554 infrared excess candidates (446 are
presented for the first time here) from 41020 white-dwarf candidates
with a Gaia magnitude of G<18.5mag. Our infrared excess candidate
sample extends to a white-dwarf temperature range of 4500-98000K and a
white-dwarf mass range of 0.1-1.2M☉. We caution that these
objects should be treated as infrared excess candidates until
confirmed with other methods.
We present a three-fold increase in the sample of white dwarfs known
to have infrared excesses. Among the sample applications is the study
of the accretion of planetary material by white dwarfs and the
identification of new white-dwarf-brown-dwarf pairs.
Description:
The first systematic identification of cool infrared excess around
white dwarfs became possible after the launch of the Spitzer Space
Telescope. Several studies have increased the number of
Spitzer-confirmed white dwarfs, (Farihi et al., 2010ApJ...714.1386F 2010ApJ...714.1386F;
Barber et al., 2016MNRAS.459.1415B 2016MNRAS.459.1415B 2016; Dennihy et al.,
2020ApJ...891...97D 2020ApJ...891...97D; Melis et al. HST Proposal, Cycle 28, ID. #16169;
Lai et al., 2021ApJ...920..156L 2021ApJ...920..156L).
A total of 107 white dwarfs (with G≤17mag) with an infrared excess
have been identified so far. This modest sample extends over a wide
range of space parameters, with a temperature range from 7300 to
34000K and a mass range from 0.3 to 1.2 solar mass (Table 1).
WISE has a beam size of 6", which is much larger than the Gaia
resolution (on the order of milliarcseconds). The matching by
coordinates that we performed between the two catalogs would not be
able to detect a false-positive infrared excess due to a background
source within the WISE beam (i.e., within 3" of the Gaia white
dwarf).
To exclude such contamination, we cross-matched the WISE coordinates
of Sample C with the entire (not just white dwarfs) Gaia EDR3 catalog.
Hence, we verified whether more than one Gaia source (i.e., potential
an infrared emitter) lay within 3" of the WISE coordinates. We found
two or more Gaia sources within the WISE beam in 1740 cases. These
were excluded from Sample C as potentially contaminated infrared
sources.
Additionally, we excluded 111 sources lacking effective temperature
and log g values in the Gaia catalog. As these values are required for
the next selection step, these sources were removed. This left a final
sample of 9893 white dwarfs (Sample D, table 3) to be checked for a
potential infrared excess.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 107 108 Bright white dwarfs (G≤17mag) confirmed to have
infrared excess
table3.dat 126 9893 Sample D, specifying those sources with infrared
excesses (Sample F), as well as the contaminated
sources (the ones excluded in the step from
Sample E to Sample F)
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
II/365 : CatWISE2020 catalog (updated version 28-Jan-2021) (Marocco+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Type Object type (1)
3- 30 A28 -- Name SIMBAD name
32- 44 F13.9 deg RAdeg Right ascension from Gaia DR2 catalog
(ICRS) at Ep=2015.5
46- 58 F13.9 deg DEdeg Declination from Gaia DR2 catalog
(ICRS) at Ep=2015.5
60- 64 F5.2 mag Gmag Gaia G magnitude
67- 75 A9 -- IRExs IR Excess assesment in our work (2)
77-107 A31 -- Ref Reference where the observation is reported (3)
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Note (1): Object type as follows:
1 = Dusty disks
2 = White Dwarf+main sequence/M dwarf
3 = White Dwarf+Brown dwarf
Note (2): N = There is no CatWISE photometry.
Note (3): Dust disks, white-dwarf-main sequence or M dwarf are confirmed by
Spitzer observations, and the white-dwarf-brown-dwarf pairs do not
have Spitzer observations, so we list the discovery paper.
References as follows:
Barber2016 = 2016MNRAS.459.1415B 2016MNRAS.459.1415B, Cat J/MNRAS/549/1415
Bergfors2014 = 2014MNRAS.444.2147B 2014MNRAS.444.2147B
Brinkworth2009 = 2009ApJ...696.1402B 2009ApJ...696.1402B
Brinkworth2012 = 2012ApJ...750...86B 2012ApJ...750...86B
Dennihy2020 = 2020ApJ...891...97D 2020ApJ...891...97D
Farihi&Christopher2004 = 2004AJ....128.1868F 2004AJ....128.1868F
Farihi+2015 = 2015sptz.prop11182F
Farihi2008a = 2008ApJ...674..431F 2008ApJ...674..431F
Farihi2009 = 2009ApJ...694..805F 2009ApJ...694..805F
Farihi2010 = 2010ApJ...714.1386F 2010ApJ...714.1386F
Farihi2011 = 2011ApJ...728L...8F 2011ApJ...728L...8F
Girven2012 = 2012ApJ...749..154G 2012ApJ...749..154G
Jura2007 = 2007ApJ...663.1285J 2007ApJ...663.1285J
Jura2009IR = 2009AJ....137.3191J 2009AJ....137.3191J
Kilic&Redfield2007 = 2007ApJ...660..641K 2007ApJ...660..641K
Kilic2012 = 2012MNRAS.419L..59K 2012MNRAS.419L..59K
Lai2021 = 2021ApJ...920..156L 2021ApJ...920..156L
Maxted2006 = 2006Natur.442..543M 2006Natur.442..543M
Melis2020 = 2020ApJ...905...56M 2020ApJ...905...56M
Reach2005 = 2005ApJ...635L.161R 2005ApJ...635L.161R
Rocchetto2015 = 2015MNRAS.449..574R 2015MNRAS.449..574R, Cat. J/MNRAS/449/574
Steele2013 = 2013MNRAS.429.3492S 2013MNRAS.429.3492S
Swan2020 = 2020MNRAS.496.5233S 2020MNRAS.496.5233S
Vanderburg2015 = 2015Natur.526..546V 2015Natur.526..546V
Wang2019 = 2019ApJ...886L...5W 2019ApJ...886L...5W
Wilson2019 = 2019MNRAS.487..133W 2019MNRAS.487..133W
Xu2015 = 2015ApJ...806L...5X 2015ApJ...806L...5X, Cat. J/ApJ/743/138
XuJura2012 = 2012ApJ...745...88X 2012ApJ...745...88X
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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- 10 F10.6 deg RAdeg Right ascension from Gaia EDR3 catalog
(ICRS) at Ep=2016.0
13- 22 F10.6 deg DEdeg Declination from Gaia EDR3 catalog
(ICRS) at Ep=2016.0
24- 27 F4.1 mag Gmag Gaia G magnitude
29- 34 I6 K Teff Effective temperature
36- 39 F4.2 [cm/s2] logg Surface gravity
41- 45 F5.2 mas plx Parallax
47- 50 F4.2 Msun Mass Mass
52- 58 A7 --- SpType Spectral type
60- 64 F5.2 mag W1mag W1 magnitude
66- 69 F4.2 mag e_W1mag W1 magnitude uncertainty
71- 75 F5.2 mag W2mag W2 magnitude
77- 80 F4.2 mag e_W2mag W2 magnitude uncertainty
82- 86 F5.2 mag W1magMod Model W1 magnitude
88- 92 F5.2 mag W2magMod Model W2 magnitude
94- 99 F6.2 --- chiW1 W1 magnitude excess
101-106 F6.2 --- chiW2 W2 magnitude excess
108-113 F6.2 --- sigmaW12 Color excess
115-126 A12 --- FinalExcess Final excess (1)
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Note (1): Final excess as follows:
Only Mag = infrared excess is identified from W1 and W2 mag excesses.
Only Color = infrared excess is identified from (W1-W2) color excess.
Color+Mag = infrared excess is identified with both methods.
Contaminated = sources rejected due to visual contamination in WISEView images
No Excess = No excess
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Acknowledgements:
Cristina Madurga Favieres, cmadurga(at)ucm.es
(End) Patricia Vannier [CDS] 17-Jun-2024