J/AJ/167/275 Warm debris disk candidates based on IR excess (Mizuki+, 2024)
Frequencies of Warm Debris Disks Based on Point Source Catalogs of
Spitzer, WISE, and Gaia.
Mizuki T., Momose M., Aizawa M., Kobayashi H.
<Astron. J. 167, 275 (2024)>
=2024AJ....167..275M 2024AJ....167..275M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, dwarfs ; Infrared sources ; Photometry, infrared
Keywords: Debris disks - Infrared excess - Spectral energy distribution -
Catalogs - Main sequence stars - Space observatories - Gaia
Abstract:
More than a thousand warm debris disks have been detected as infrared
excess at mid-infrared wavelengths, and their frequencies have been
obtained for various spectral types of stars. However, the dependence
of the frequencies on spectral type is still debated because the
number of stars with significant and detectable infrared excess is
limited. Herein, we present the largest systematic search for infrared
excess using data from Gaia, WISE, and Spitzer. We identified 373,
485, and 255-reliable infrared excesses in the mid-infrared archival
data at wavelengths of 12, 22, and 24um for WISE/W3, W4, and
Spitzer/MIPS ch1, respectively. Although we confirmed that more
massive stars tend to show higher frequencies of debris disks, these
disk frequencies are relatively flat for both low- and
intermediate-mass stars, with a jump at 7000K for all three
wavelengths. Assuming that bright, warm debris disks have lifetimes of
a few to several hundred million years, the disk frequency can be
understood as the ratio between the timescale and the upper limits of
the sample ages. We also found that intermediate-mass stars with
infrared excess tend to be bluer and fainter along the evolutionary
track than those without, implying that massive stars hosting debris
disks are relatively young, with an isochronal age of approximately
500 Myr. These tendencies are reasonably explained by a standard
scenario in which debris disks are likely to be produced by collisions
of planetesimals in the early stages of stellar evolution, such as the
Late Heavy Bombardment.
Description:
This catalog lists 1047 stars with detected mid-infrared excesses
based on a systematic analysis of archival data from Gaia eDR3, WISE
(W3 and W4), and Spitzer/MIPS 24um (M1). Excess fluxes are identified
by comparing observed fluxes with model SEDs fitted using Gaia
photometry and others.
The catalog includes basic astrometric parameters from Gaia eDR3,
photometric data, SED fitting results, debris disk flags for each
band, and detection reliability parameters including contamination and
astrophysical probabilities.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 287 1047 Catalog of 1047 stars with detected mid-infrared
excesses based on a systematic analysis of
archival data from Gaia eDR3, WISE (W3 and W4),
and Spitzer/MIPS 24um (M1)
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See also:
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
II/328 : AllWISE Data Release (Cutri+ 2013)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- GaiaEDR3 Gaia EDR3 source ID (ID_GaiaEDR3)
21- 48 A28 --- Name SIMBAD identifier (NAME_SIMBAD)
50- 56 F7.3 deg RAdeg Gaia EDR3 right ascension (ICRS)
at Ep=2016.0 (RA)
58- 64 F7.3 deg DEdeg Gaia EDR3 declination (ICRS)
at Ep=2016.0 (DEC)
66- 73 F8.3 mas/yr pmRA Proper motion in RA (PM_RA)
75- 82 F8.3 mas/yr pmDE Proper motion in Dec (PM_DEC)
84- 90 F7.3 pc Dist Distance from Gaia parallax (D)
92- 97 F6.3 mag Gmag Gaia G-band magnitude (Gmag)
99-104 F6.3 --- RUWE Renormalized Unit Weight Error (RUWE)
106-110 F5.3 --- Chi2 Reduced chi-square of SED fit (CHISQ)
112-116 I5 K Teff Stellar effective temperature (TEFF)
118-120 F3.1 [cm/s2] logg Stellar surface gravity (LOGG)
122-128 F7.3 Lsun L Stellar luminosity (L)
130 I1 --- DebrisW3 [0/1] Excess flag at WISE W3 (Debris_W3)
132 I1 --- DebrisW4 [0/1] Excess flag at WISE W4 (Debris_W4)
134 I1 --- DebrisM1 [0/1] Excess flag at WISE M1 (Debris_M1)
137-144 F8.3 mJy FW3 ?=-1 Observed flux at W3 (FLUX_W3) (1)
147-152 F6.3 mJy e_FW3 ?=-1 Uncertainty in W3 flux (FERR_W3) (1)
154-161 F8.3 mJy FmodW3 Model SED flux at W3 (FLUXMODELW3)
163-168 F6.3 mJy e_FmodW3 Uncertainty of model flux at W3
(FERRMODELW3)
170-175 F6.3 --- epsilonW3 ?=-1 Detection efficiency at W3 (epsilon_W3)
177-182 F6.3 --- pbkgW3 ?=-1 Background contamination probability
at W3 (pbkg_W3)
184-187 F4.1 --- pastrW3 ?=-1 Probability of astrophysical excess
at W3 (pastr_W3)
190-196 F7.3 mJy FW4 ?=-1 Observed flux at W4 (FLUX_W4) (1)
199-204 F6.3 mJy e_FW4 ?=-1 Uncertainty in W4 flux (FERR_W4)
206-212 F7.3 mJy FmodW4 Model SED flux at W4 (FLUXMODELW4) (1)
214-219 F6.3 mJy e_FmodW4 Uncertainty of model flux at W4
(FERRMODELW4)
221-226 F6.3 --- epsilonW4 ?=-1 Detection efficiency at W4
(epsilon_W4) (1)
228-233 F6.3 --- pbkgW4 ?=-1 Background contamination probability
at W4 (pbkg_W4)
235-238 F4.1 --- pastrW4 ?=-1 Probability of astrophysical excess
at W4 (pastr_W4)
241-246 F6.3 mJy FM1 ?=-1 Observed flux at M1 (FLUX_M1) (1)
248-253 F6.3 mJy e_FM1 ?=-1 Uncertainty in M1 flux (FERR_M1) (1)
255-261 F7.3 mJy FmodM1 Model SED flux at M1 (FLUXMODELM1)
263-268 F6.3 mJy e_FmodM1 Uncertainty of model flux at M1
(FERRMODELM1)
270-275 F6.3 --- epsilonM1 ?=-1 Detection efficiency at M1
(epsilon_M1) (1)
277-282 F6.3 --- pbkgM1 ?=-1 Background contamination probability
at M1 (pbkg_M1)
284-287 F4.1 --- pastrM1 ?=-1 Probability of astrophysical excess
at M1 (pastr_M1)
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Note (1): Values of -1 indicate missing or invalid measurements.
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Acknowledgements:
Toshiyuki Mizuki, toshiyuki.mizuki.astr(at)gmail.com
(End) Patricia Vannier [CDS] 28-Nov-2025