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J/ApJ/837/15    WISE IR excesses among main sequence stars    (Da Costa+, 2017)

On the incidence of WISE Infrared excess among solar analog, twin, and sibling stars. Da Costa A.D., Canto Martins B.L., Leao I.C., Lima Jr J.E., Freire da Silva D., de Freitas D.B., de Medeiros J.R. <Astrophys. J., 837, 15-15 (2017)> =2017ApJ...837...15D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, G-type ; Photometry, infrared Keywords: circumstellar matter; infrared: stars; stars: individual: HD 86087; stars: solar-type Abstract: This study presents a search for infrared (IR) excess in the 3.4, 4.6, 12, and 22µm bands in a sample of 216 targets, composed of solar sibling, twin, and analog stars observed by the Wide-field Infrared Survey Explorer (WISE) mission. In general, an IR excess suggests the existence of warm dust around a star. We detected 12µm and/or 22µm excesses at the 3σ level of confidence in five solar analog stars, corresponding to a frequency of 4.1% of the entire sample of solar analogs analyzed, and in one out of 29 solar sibling candidates, confirming previous studies. The estimation of the dust properties shows that the sources with IR excesses possess circumstellar material with temperatures that, within the uncertainties, are similar to that of the material found in the asteroid belt in our solar system. No photospheric flux excess was identified at the W1 (3.4µm) and W2 (4.6µm) WISE bands, indicating that, in the majority of stars of the present sample, no detectable dust is generated. Interestingly, among the 60 solar twin stars analyzed in this work, no WISE photospheric flux excess was detected. However, a null-detection excess does not necessarily indicate the absence of dust around a star because different causes, including dynamic processes and instrument limitations, can mask its presence. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 173 216 Stellar parameters, including V, 2MASS and WISE magnitudes and excess significance χλ for the four WISE bands of the 216 Sun-like stars
See also: I/259 : The Tycho-2 Catalogue (Hog+ 2000) II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) V/117 : Geneva-Copenhagen Survey of Solar neighbourhood (Holmberg+, 2007) V/139 : The SDSS Photometric Catalog, Release 9 (Adelman-McCarthy+, 2012) II/328 : AllWISE Data Release (Cutri+ 2013) J/ApJ/497/330 : Candidate main-sequence stars (Mannings+, 1998) J/A+AS/141/371 : Low-mass stars isochrones (Girardi+, 2000) J/A+A/365/545 : Remnant disks around MS stars IR flux (Habing+, 2001) J/AJ/124/1670 : Post-T Tauri Stars in Sco-Cen Association (Mamajek+, 2002) J/ApJ/620/1010 : Spitzer 24µm photometry of A dwarfs (Rieke+, 2005) J/ApJ/636/1098 : Debris disks around solar-type stars (Bryden+, 2006) J/AJ/132/161 : NStars project: The southern sample. I. (Gray+, 2006) J/ApJ/653/675 : Spitzer 24µm photometry of A dwarfs (Su+, 2006) J/A+A/492/277 : Analysis of Collinder 69 stars with VOSA (Bayo+, 2008) J/MNRAS/427/343 : Infrared excesses of Hipparcos stars (McDonald+, 2012) J/ApJ/750/98 : 24um observations of AFGKM stars of 3 clusters (Urban+, 2012) J/ApJ/775/55 : Spitzer IR excesses in A-K stars (Ballering+, 2013) J/A+A/555/A11 : DUNES survey observational results (Eiroa+, 2013) J/ApJ/768/25 : Spitzer & Herschel obs. of debris disks (Gaspar+, 2013) J/ApJS/208/29 : HIP stars with 22µm excess (Wu+, 2013) J/ApJS/211/25 : Spitzer/IRS debris disk catalog. I. (Chen+, 2014) J/MNRAS/437/391 : IR excess in Sun-like stars from WISE (Cruz-Saenz+, 2014) J/AJ/148/3 : Debris disk candidates detected with AKARI/FIS (Liu+, 2014) J/ApJS/212/10 : WISE IR excesses for stars within 75pc (Patel+, 2014) J/ApJ/787/154 : Elemental abundances of solar sibling cand. (Ramirez+, 2014) J/ApJ/785/33 : F4-K2 stars high quality Spitzer/MIPS obs. (Sierchio+, 2014) J/A+A/574/A124 : Spectroscopy of solar twins and analogues (Datson+, 2015) J/A+A/575/A51 : Line lists in Sun siblings (Liu+, 2015) J/ApJS/225/15 : IR excess stars from Tycho-2 and AllWISE (Cotten+, 2016) J/A+A/593/A51 : Debris discs around nearby FGK stars (Montesinos+, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 18 A18 --- Type Solar type (1) 20- 28 A9 --- Name Star identifier (HD or HIP number) 30- 34 F5.2 mag Vmag [3.8/15] The V band magnitude 36- 45 A10 --- SpType MK spectral type 47- 51 I5 K Teff [3925/10500]? Effective temperature 53- 58 F6.2 K e_Teff [4/110]? Uncertainty in Teff 60- 63 F4.2 [cm/s2] log(g) [3.2/5.4]? Log surface gravity 65- 70 F6.2 [cm/s2] e_log(g) [0.01/3]? Uncertainty in log(g) 72- 77 F6.3 [Sun] [Fe/H] [-0.5/0.4]? Metallicity 79- 83 F5.3 [Sun] e_[Fe/H] [0.004/0.1]? Uncertainty in [Fe/H] 85- 97 A13 --- Ref Reference codes (2) 99-103 F5.2 mag Jmag [3.6/13.6] 2MASS J band magnitude 105-109 F5.2 mag Hmag [3.5/13.2] 2MASS H band magnitude 111-115 F5.2 mag Kmag [3.5/13.1] 2MASS Ks band magnitude 117-121 F5.2 mag W1mag [3.4/13.2] WISE 3.4um (W1) band magnitude 123-127 F5.2 mag W2mag [3.1/13.2] WISE 4.6um (W2) band magnitude 129-133 F5.2 mag W3mag [2.5/12.5] WISE 12um (W3) band magnitude 135-139 F5.3 mag W4mag [0.01/9.1]? WISE 22um (W4) band magnitude 141-146 F6.3 --- chi3.4 [-6/8.3] Excess significance at 3.4um (3) 148-153 F6.3 --- chi4.6 [-4.7/7.5] Excess significance at 4.6um (3) 155 A1 --- l_chi12 Limit flag on chi12 158-163 F6.3 --- chi12 [-3/20.1] Excess significance at 12um (3) 165 A1 --- l_chi22 Limit flag on chi22 168-173 F6.3 --- chi22 [-1.7/17]? Excess significance at 22um (3)
Note (1): Object type as follows: Siblings = Solar siblings: stars that were born simultaneously with the Sun (6 occurrences) Siblings candidates = Solar siblings candidates (29 occurrences) Twins = Solar twins: stars with high-resolution, high signal-to-noise ratio (S/N) spectra that are identical to the spectrum of the Sun, regardless of their origin (60 occurrences) Analogs = Solar analogs: stars that are spectroscopically similar to the Sun and that are known to have stellar properties close to solar values (121 occurrences) Note (2): Reference for Vmag, SpType, Teff, logg, [Fe/H] as follows: 1 = Hipparcos (ESA 1997, I/239); 2 = Datson et al. (2015, J/A+A/574/A124); 3 = Hog et al. (2000, I/259); 4 = Houk & Swift (1999, III/214); 5 = Ramirez et al. (2012ApJ...752....5R); 6 = Ramirez et al. (2014, J/ApJ/787/154); 7 = Pasquini et al. (2008A&A...489..677P); 8 = Liu et al. (2015, J/A+A/575/A51); 9 = Ducati (2002, II/237); 10 = Gray et al. (2006, J/AJ/132/161); 11 = Chen et al. (2014, J/ApJS/211/25); 12 = Stauffer et al (1995ApJ...454..910S); 13 = Nordstrom et al. (2004, V/117; superseded by V/130); 14 = Chen et al. (2006ApJS..166..351C); 15 = Batista et al. (2014A&A...564A..43B); 16 = Saffe et al. (2008A&A...490..297S); 17 = Henden et al (2016, II/336); 18 = Houk & Smith-Moore (1988, III/133). Note (3): Measurements of the WISE IR excess for each source were made using the excess significance χλ (Beichman+ 2006ApJ...652.1674B), which can be defined as Equation (1): (Fλobs-Fλphot)/(σobs2cal2)0.5 where Fλobs is the observed flux value in the [3.4], [4.6], [12], or [22] bands; Fλphot is the theoretical photospheric flux value at the same wavelength computed from photospheric modeling; σobs represents the errors at F_λobs and σcal are the absolute calibration uncertainties of the WISE estimated at 2.4%, 2.8%, 4.5%, and 5.7% in the [3.4], [4.5], [12], and [22] bands, respectively. See section 2.1.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 10-Oct-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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