J/AJ/148/3 Debris disk candidates detected with AKARI/FIS (Liu+, 2014)
Bright debris disk candidates detected with the AKARI/Far-infrared surveyor.
Liu Q., Wang T., Jiang P.
<Astron. J., 148, 3 (2014)>
=2014AJ....148....3L 2014AJ....148....3L
ADC_Keywords: Infrared sources ; Photometry, UBV ; Photometry, infrared
Keywords: catalogs - circumstellar matter - infrared: stars
Abstract:
We cross-correlate the Hipparcos main-sequence star catalog with the
AKARI/FIS catalog and identify 136 stars (at >90% reliability) with
far-infrared detections in at least one band. After rejecting 57 stars
classified as young stellar objects, Be stars and other type stars
with known dust disks or with potential contaminations, and 4 stars
without infrared excess emission, we obtain a sample of 75 candidate
stars with debris disks. Stars in our sample cover spectral types from
B to K with most being early types. This represents a unique sample of
luminous debris disks that derived uniformly from an all-sky survey
with a spatial resolution factor of four better than the previous such
survey by IRAS. Moreover, by collecting the infrared photometric data
from other public archives, almost three-quarters of them have
infrared excesses in more than one band, allowing an estimate of the
dust temperatures. We fit the blackbody model to the broadband
spectral energy distribution of these stars to derive the statistical
distribution of the disk parameters. Four B stars with excesses in
four or more bands require a double blackbody model, with the high one
around 100 or 200K and the low one around 40-50K.
Description:
In this paper, we search systematically for debris systems around
main-sequence stars by cross-correlating the Hipparcos catalog (cat.
I/239) with the AKARI/Far-Infrared Surveyor (AKARI/FIS) All-Sky Survey
Bright Source Catalogue (cat. II/298).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 24 61 List of rejected sources
table2.dat 133 75 Photometry and flux density for all sources
table3.dat 89 55 Star basic properties and dust basic properties
of our sample sources (group II)
--------------------------------------------------------------------------------
See also:
II/328 : AllWISE Data Release (Cutri+ 2013)
II/298 : AKARI/FIS All-Sky Survey Point Source Catalogues (ISAS/JAXA, 2010)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
J/ApJ/660/1556 : Characterization of dusty debris disks (Rhee+, 2007)
J/ApJ/653/675 : Spitzer 24um photometry of A dwarfs (Su+, 2006)
J/ApJ/620/1010 : Spitzer 24um photometry of A dwarfs (Rieke+, 2005)
J/A+A/365/545 : Remnant disks around main-sequence stars IR flux
(Habing+, 2001)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 I6 --- HIP HIP number (cat. I/239)
7 A1 --- f_HIP [ab] Note: a=Stars in nebula;
b=Rejected by diffuse WISE images
9- 22 A14 --- AKARI AKARI/FIS identification
24 I1 --- Rej Reason for rejection (1)
--------------------------------------------------------------------------------
Note (1): Reason for rejection defined as follows:
1 = O star;
2 = Be star;
3 = Young stellar object (YSO) or pre-main-sequence (PMS) star;
4 = Contamination;
5 = Post asymptotic-giant-branch (AGB) star;
6 = Quasar;
7 = AKARI/FIS flux density is not reliable (flux density quality flag "1"
in AKARI/FIS 4 bands);
8 = No far-infrared excess.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 I6 --- HIP [746/118289] Hipparcos number (cat. I/239)
8- 12 F5.2 mag Bmag [0.03/10.38] Hipparcos B band magnitude
14- 18 F5.2 mag Vmag [0.03/10.4] Hipparcos V band magnitude
20- 24 F5.2 mag Jmag [-0.18/10.32] 2MASS J band magnitude
26- 30 F5.2 mag Hmag [-0.03/10.31] 2MASS H band magnitude
32- 36 F5.2 mag Kmag [0.13/10.25] 2MASS Ks band magnitude
38 I1 --- f_Jmag [1/3] Jmag quality flag (1)
39 I1 --- f_Hmag [1/3] Hmag quality flag (1)
40 I1 --- f_Kmag [1/3] Kmag quality flag (1)
42- 46 F5.2 mag W1mag [-2.1/10.2] WISE W1 magnitude
48- 52 F5.2 mag W2mag [-2.1/10.0] WISE W2 magnitude
54- 57 F4.2 mag W3mag [0.02/8.6] WISE W3 magnitude
59- 63 F5.2 mag W4mag [-0.2/8.0] WISE W4 magnitude
65- 68 F4.2 --- W1sat [0/1] Saturated pixel fraction, W1
70- 73 F4.2 --- W2sat [0/1] Saturated pixel fraction, W2
75- 78 F4.2 --- W3sat [0/1] Saturated pixel fraction, W3
80- 83 F4.2 --- W4sat [0/1] Saturated pixel fraction, W4
85- 89 F5.2 Jy S65 [0.08/15.72]? AKARI/FIS 65µm flux density
91- 94 A4 --- n_S65 [null] null S65 value
96-100 F5.2 Jy S90 [0.2/12.1] AKARI/FIS 90µm flux density
102-105 F4.2 Jy S140 [0/7.78]? AKARI/FIS 140µm flux density
107-110 A4 --- n_S140 [null] null S140 value
112-115 F4.2 Jy S160 [0.01/6.26]? AKARI/FIS 160µm flux density
117-120 A4 --- n_S160 [null] null S160 value
122 I1 --- f_S65 [1/3] Flux density quality flag in S65 (2)
124 I1 --- f_S90 [1/3] Flux density quality flag in S90 (2)
126 I1 --- f_S140 [0/3] Flux density quality flag in S140 (2)
128 I1 --- f_S160 [1/3] Flux density quality flag in S160 (2)
130-133 F4.1 arcsec Off [2/20] AKARI/FIS position offset
--------------------------------------------------------------------------------
Note (1): The read flag from 2MASS catalog (cat. II/246) indicates the source
of J,H,K "default" magnitudes as a 3-digit integer, where the 1st digit
corresponds to the J band, the 2nd to the H band, and the 3rd to the Ks
band. Values of "1", "2" or "3" generally indicate the best quality
photometry.
Note (2): Flux density quality flag defined as follows:
0 = Not observed (no scan data available);
1 = The source is not confirmed;
2 = The source is confirmed but flux is not reliable (see FLAGS);
3 = High quality (the source is confirmed and flux is reliable).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 I6 --- HIP [4683/118289] HIP number (cat. I/239) (1)
7 A1 --- f_HIP [a] SED fitting with two blackbody model
9- 14 I6 --- HD [5839/232344]? HD number
16- 20 F5.1 pc Dist [7/764] Distance
22- 26 I5 K Teff [4750/20000] Effective temperature
28- 30 F3.1 [cm/s2] logg [4/4.5] Log surface gravity
32- 36 F5.3 mag E(B-V) [0/0.2] Reddening
38- 40 I3 K Tdust [27/194] Dust temperature (see Section 3.2.1)
42- 45 I4 AU Rdust [4/2500] Radius of dust ring (2)
47- 54 E8.3 Mgeo Mdust [0.0245/348] Total dust mass; in earth mass (3)
56- 63 E8.3 --- Ldust Dust fractional luminosity (4)
65- 72 A8 --- SpT Spectral type
74- 89 A16 --- Ref Reference(s) (5)
--------------------------------------------------------------------------------
Note (1): According to the number of bands with detected far-infrared and
mid-infrared excesses (AKARI/FIS 4 bands and WISE 12µm and 22µm), we
further divide the infrared excess sample into two groups: infrared excess
in a single band (Group I) and excesses in two or more bands (Group II).
See Section 3 for more details.
Note (2): Rdust=(278/Tdust)2(L*/L☉)0.5 (Eq. (6)).
See Section 3.2.3 for more details.
Note (3): Mdust=Ldust(Rdust2/9.12)M⊕ (Eq. (10)).
See 3.2.3 for details.
Note (4): Fractional luminosity is defined as the ratio of infrared luminosity
of the debris disk to that of the star, frequently used to characterize the
effective optical depth of the disk, Ldust=Lir/L* (Eq. (5)), where
Lir is the infrared luminosity estimated by the fitted infrared blackbody
model. The stellar luminosity L* is calculated from the best-fit
Kurucz model. See Section 3.2.2 for more details.
Note (5): Reference as follows:
1 = Oudmaijer et al. (1992A&AS...96..625O 1992A&AS...96..625O);
2 = Rhee et al. (2007, cat. J/ApJ/660/1556);
3 = Koerner et al. (1998ApJ...503L..83K 1998ApJ...503L..83K);
4 = Chen et al. (2006ApJS..166..351C 2006ApJS..166..351C);
5 = Decin et al. (2003ApJ...598..636D 2003ApJ...598..636D);
6 = Habing et al. (1999Natur.401..456H 1999Natur.401..456H);
7 = Habing et al. (2001, cat. J/A+A/365/545);
8 = Su et al. (2006, cat. J/ApJ/653/675);
9 = Carpenter et al. (2008ApJS..179..423C 2008ApJS..179..423C);
10 = Moor et al. (2006ApJ...644..525M 2006ApJ...644..525M);
11 = Moor et al. (2011ApJS..193....4M 2011ApJS..193....4M);
12 = Rebull et al. (2008ApJ...681.1484R 2008ApJ...681.1484R);
13 = Rieke et al. (2005, cat. J/ApJ/620/1010).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Sylvain Guehenneux [CDS] 21-Nov-2014