J/ApJ/705/89 IRS spectra of solar-type stars (Lawler+, 2009)
Explorations beyond the snow line: Spitzer/IRS spectra of debris disks around
solar-type stars
Lawler S.M., Beichman C.A., Bryden G., Ciardi D.R., Tanner A.M., Su K.Y.L.,
Stapelfeldt K.R., Lisse C.M., Harker D.E.
<Astrophys. J., 705, 89-111 (2009)>
=2009ApJ...705...89L 2009ApJ...705...89L
ADC_Keywords: Stars, nearby ; Stars, G-type ; Spectra, infrared
Keywords: infrared: stars - circumstellar matter - planetary systems -
Kuiper Belt
Abstract:
We have observed 152 nearby solar-type stars with the Infrared
Spectrometer (IRS) on the Spitzer Space Telescope. Including stars
that met our criteria but were observed in other surveys, we get an
overall success rate for finding excesses in the long-wavelength IRS
band (30-34um) of 11.8%±2.4%. The success rate for excesses in the
short-wavelength band (8.5-12um) is ∼1% including sources from other
surveys. Two stars (HD 40136 and HD 10647) show weak evidence for
spectral features; the excess emission in the other systems is
featureless. For most stars with excesses, we detect an excess at both
IRS and Multiband Imaging Photometer for Spitzer (MIPS) wavelengths.
Only three stars in this sample show a MIPS 70um excess with no IRS
excess, implying that very cold dust is rare around solar-type stars.
Description:
We observed each star with all four wavelength modules of the IRS:
short-low orders 2 and 3 (SL2; 5.1-7.5um, SL3; 7.1-8.4um), short-low
order 1 (SL1; 7.5-14.0um), long-low order 2 (LL2; 14.0-20.5um), and
long-low order 1 (LL1; 20-34um), as part of the Spitzer GO program
20463 (PI: D. Ciardi).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 140 152 Basic data of the nearby solar-type stars sample
table4.dat 73 152 IRS data for the sample
spectra/* . 16 Spitzer/IRS spectra for stars with excess
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See also:
B/pastel : The PASTEL catalogue (Soubiran+, 2010-)
V/117 : Geneva-Copenhagen Survey of Solar neighbourhood (Holmberg+, 2007)
II/237 : Stellar Photometry in Johnson's 11-color system (Ducati, 2002)
III/193 : Chemical Abundances in Late-Type Stars (Thevenin, 1998)
V/89 : Ages, Metallicities, Galactic Orbit of F stars (Marsakov+ 1995)
V/58 : [Fe/H], Vel, Orbits of F2-K5 Dwarfs 80pc from Sun (Marsakov+ 1988)
II/7 : UBVRIJKLMNH Photoelectric Catalogue (Morel+ 1978)
II/5 : UBV Photometry of Bright Stars (Johnson+ 1966)
J/ApJS/159/141 : Spectroscopic properties of cool stars. I. (Valenti+, 2005)
J/AZh/82/453 : Catalogue of spectroscopic abundances in stars (Borkova+,
2005)
J/ApJS/152/261 : Chromospheric Ca II emission in nearby stars (Wright+, 2004)
J/MNRAS/349/757 : Masses, ages and metallicities of F-G dwarfs (Lambert+, 2004)
J/AJ/125/3311 : JHKL'M photometry of northern bright stars (Kidger+, 2003)
J/A+A/398/731 : [Fe/H] catalog of class IV-V stars (Taylor, 2003)
J/A+A/384/491 : Nearby solar-type stars. I. (Cutispoto+, 2002-03)
J/A+A/394/927 : Age-metallicity relation for nearby stars (Ibukiyama+, 2002)
J/MNRAS/326/959 : Empirical calibration of the near-IR Ca triplet (Cenarro+,
2001)
J/A+A/377/911 : Age-metallicity relation in solar neighbourhood (Feltzing+,
2001)
J/A+A/348/897 : Ages of main-sequence stars (Lachaume+, 1999)
J/MNRAS/298/332 : Chromospheric activity-age relation (Rocha-Pinto+ 1998)
J/AJ/115/2397 : Stars in the solar region (Eggen 1998)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [HD]
4- 9 I6 --- HD HD number
10 A1 --- pl [c] c: star has at least one known radial
velocity planet
12- 17 I6 --- HIP ? HIP number
19- 25 A7 --- GJ GJ (Gliese-Jahreiss) designation
27- 32 A6 --- SpType SIMBAD MK spectral type
34- 37 I4 K Temp Effective temperature
39- 42 F4.1 pc Dist Heliocentric distance
44- 47 F4.2 mag Vmag SIMBAD V-band magnitude
49- 52 F4.2 mag Ksmag 2MASS Ks-band magnitude unless flagged
53- 55 A3 --- f_Ksmag [b,d ] Non-2MASS or low quality (1)
57- 60 F4.1 Gyr Age ? Average age (2)
61 A1 --- f_Age [e] Flag for HD 10647 (3)
63- 66 F4.1 Gyr b_Age ? Minimum age
68- 71 F4.1 Gyr B_Age ? Maximum age
73- 89 A17 --- r_Age Age reference(s) (4)
91- 95 F5.2 [Sun] [Fe/H] ? Average Fe/H
97-100 F4.2 [Sun] e_[Fe/H] ? 1σ uncertainty in [Fe/H]
102-137 A36 --- r_[Fe/H] References for [Fe/H] (4)
139-140 A2 --- Sp [Sp] spectrum available in the "spectra"
subdirectory (shows excess)
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Note (1): Flag(s) as follows:
b = Star has J, H and/or K values from Johnson et al. (1966, Cat. II/5)
or other literature.
d = Star has one or more bad 2MASS values (error >20%), slightly reducing
the accuracy of its photometric model.
Note (2): Age from Wright et al. (2004, Cat. J/ApJS/152/261) or Valenti &
Fischer (2005, Cat. J/ApJS/159/141) if available, otherwise an average
of literature values.
Note (3):
e = After considering several factors, our age for HD 10647 comes from
Chen et al. (2006ApJS..166..351C 2006ApJS..166..351C; see note in Section 2).
Minimum and maximum ages for this star are from all literature sources.
Note (4): References as follows:
B = Borkova & Marsakov 2005, Cat. J/AZh/82/453
Ba = Barry 1988ApJ...334..436B 1988ApJ...334..436B
Bo = Borges et al. 1995AJ....110.2408B 1995AJ....110.2408B
C = Chen et al. 2001, Cat. J/A+A/371/943
Ch = Chen et al. 2006ApJS..166..351C 2006ApJS..166..351C
CS = Cayrel de Strobel et al. 1996 (Cat. III/200); 2001 (Cat. III/221);
superseded by Cat. B/pastel
Ce = Cenarro et al. 2001, Cat. J/MNRAS/326/959
D = Ducati 2002, Cat. II/237
E = Eggen 1998, Cat. J/AJ/115/2397
F = Feltzing et al. 2001, Cat. J/A+A/377/911
I = Ibukiyama & Arimoto 2002, Cat. J/A+A/394/927
K = Kidger & Martin-Luis 2003, Cat. J/AJ/125/3311
L = Lambert & Reddy 2004, Cat. J/MNRAS/349/757
La = Lachaume et al. 1999, Cat. J/A+A/348/897
Le = Lebreton et al. 1999A&A...350..587L 1999A&A...350..587L
M = Marsakov & Shevelev 1988 (Cat. V/58); 1995 (Cat. V/89)
Ms = Mashonkina & Gehren 2001A&A...376..232M 2001A&A...376..232M
Ml = Morel & Magnenat 1978, Cat. II/7
N = Nordstrom et al. 2004, Cat. V/117
P = Perrin et al. 1977A&A....54..779P 1977A&A....54..779P
R = Randich et al. 1999A&A...348..487R 1999A&A...348..487R
RP = Rocha-Pinto & Maciel 1998, Cat. J/MNRAS/298/332
S = Sylvester & Mannings 2000MNRAS.313...73S 2000MNRAS.313...73S
T = Taylor 2003, Cat. J/A+A/398/731
Th = Thevenin 1998, Cat. III/193
V = Valenti & Fischer 2005, Cat. J/ApJS/159/141
W = Wright et al. 2004, Cat. J/ApJS/152/261
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [HD]
4- 9 I6 --- HD HD number
11- 15 A5 --- Rem [b-h, ] Note on the Spitzer photometry (1)
17- 22 F6.1 mJy Exc10 8.5-12um excess
24- 26 F3.1 mJy e_Exc10 Exc10 uncertainty
28- 33 F6.3 --- fExc10 8.5-12um fractional excess (2)
35- 38 F4.1 --- chi10 χ for excess significance (2)
40 A1 --- l_L10 Limit flag on L10
42- 45 F4.1 10-5 L10 Ldust/L* at 8.5-12um range (3)
47- 50 F4.1 mJy Exc32 30-34um excess
52- 54 F3.1 mJy e_Exc32 Exc32 uncertainty
56- 61 F6.3 --- fExc32 30-34um fractional excess (2)
63- 66 F4.1 --- chi32 χ for excess significance (2)
68 A1 --- l_L32 Limit flag on L32
70- 73 F4.1 10-5 L32 Ldust/L* at 30-34um range (3)
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Note (1): Flag as follows:
b = Star has public MIPS 24 and 70um data that was reduced as described in
Section 3.2.
c = Star has MIPS 24 and 70um data from the FGK survey (Beichman et al.
2006ApJ...639.1166B 2006ApJ...639.1166B).
d = Star has MIPS 24 and 70um data from the SIM/TPF survey (Beichman et al.
2006ApJ...652.1674B 2006ApJ...652.1674B).
e = Data has significant pointing errors or a close companion so IRS data
may not be accurate.
f = Star has MIPS 24 and 70um data from Plavchan et al.
(2009ApJ...698.1068P 2009ApJ...698.1068P).
g = Star has MIPS 24 and 70um data from Trilling et al. (2008ApJ...674.1086T 2008ApJ...674.1086T)
h = IRS data has been co-added with IRS data from the FGK or SIM/TPF program
(see Table 3).
Note (2): The fractional excess is defined as
[Fν(Observed)-Fν(Photosphere)]/Fν(Photosphere).
To assess the significance of any possible excess, we define χ10
and χ32 as [Fν(Observed)-Fν(Photosphere)]/Noise
for the two photometric bands, where Noise is a combination of the
dispersion in the fractional excess of the individual spectrum and
the population-averaged dispersion: 1% (8.5-12um) and 2% (30-34um).
For a star to have an excess, we require χ>3 for an IRS-only
detection or χ>2 if the star also has a MIPS 70um excess. See
section 4 for further details.
Note (3): Limits on Ldust/L* from using Equation (1) and three times
the dispersion in the fractional excess of the whole population.
Average values of Ldust/L* (3σ limits or detections) after
2σ rejection of outliers are 11±4 at 8.5-12um and 1.3+/0.5 at
30-34um.
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Byte-by-byte Description of file: spectra/*
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Bytes Format Units Label Explanations
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1- 6 F6.3 um lambda Wavelength λ
8- 13 F6.4 Jy Fnu Flux at λ
15- 21 F7.4 Jy Exc Excess
23- 28 F6.4 Jy e_Exc Error in Exc
30- 36 F7.4 --- fExc Fractional excess
38- 43 F6.4 --- e_fExc Error in Frac
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 30-Nov-2011