J/ApJ/630/381 Mid-IR imaging in ρ Oph (Barsony+, 2005)
A mid-infrared imaging survey of embedded young stellar objects in the
ρ Ophiuchi cloud core.
Barsony M., Ressler M.E., Marsh K.A.
<Astrophys. J., 630, 381-399 (2005)>
=2005ApJ...630..381B 2005ApJ...630..381B
ADC_Keywords: Infrared sources ; Interstellar medium ; Stars, pre-main sequence
Keywords: infrared: stars - ISM: individual (ρ Ophiuchi Cloud) -
planetary systems: protoplanetary disks - stars: formation -
stars: pre-main-sequence - surveys
Abstract:
Results of a comprehensive, new, ground-based mid-infrared imaging
survey of the young stellar population of the ρ Ophiuchi cloud are
presented. Data were acquired at the Palomar 5m and at the Keck 10m
telescopes with the MIRLIN (Mid-InfraRed Large-well Imager) and LWS
(Long Wavelength Spectrometer centered at 12.5µm) instruments, at
0.5" and 0.25" resolutions, respectively. Of 172 survey objects, 85
were detected. Among the 22 multiple systems observed, 15 were
resolved and their individual component fluxes determined.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 111 231 Mid-infrared fluxes for ρ Oph sources
table3.dat 129 37 Mid-infrared variables in Ophiuchus
table4.dat 132 176 ρ Oph source properties
table5.dat 71 39 Mid-infrared observations of known
binary/multiple systems in Ophiuchus
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See also:
J/ApJS/112/109 : Rho Oph Near-IR Positions and Photometry (Barsony+, 1997)
J/ApJ/438/813 : Stellar population in ρ Oph cloud core (Strom+, 1995)
J/AJ/130/1733 : Optical spectroscopy of ρ Oph stars (Wilking+, 2005)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- BKLT Source designations (G1)
15 A1 --- n_BKLT Note on BKLT (1)
17- 34 A18 --- OName Alias or other name
36 A1 --- n_OName Note on OName (1)
38- 39 I2 h RAh ? Hour of Right Ascension (J2000)
41- 42 I2 min RAm ? Minute of Right Ascension (J2000)
44- 48 F5.2 s RAs ? Second of Right Ascension (J2000)
50 A1 --- DE- Sign of the Declination (J2000)
51- 52 I2 deg DEd ? Degree of Declination (J2000)
54- 55 I2 arcmin DEm ? Arcminute of Declination (J2000)
57- 60 F4.1 arcsec DEs ? Arcsecond of Declination (J2000)
62- 63 A2 --- l_F10.8um [≤] Upper limit flag on F10.8um (3σ)
65- 71 F7.4 Jy F10.8um ? The 10.8µm flux
73- 74 A2 --- l_F12.5um [≤] Upper limit flag on F12.5um (3σ)
76- 80 F5.3 Jy F12.5um ? The 12.5µm flux (2)
82- 86 F5.3 Jy F12.5um2 ? Second 12.5µm flux (2)
88- 97 A10 "DD/MM/YYYY" ObsDate Observation date
99-111 A13 --- Tel The Telescope/Instrument used
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Note (1): Flag on BKLT, defined as follows:
4 = Spectroscopically determined background giant
(Luhman & Rieke 1999ApJ...525..440L 1999ApJ...525..440L);
5 = The secondary in the DoAr24E system is an Infrared Companion discovered
by Chelli et al. (1988A&A...207...46C 1988A&A...207...46C).
6 = WL16 and its extended PAH & VSG disk are thoroughly discussed in
Ressler & Barsony (2003ApJ...584..832R 2003ApJ...584..832R); the aperture photometry
presented here was measured in r=4" and r=3.75" circular apertures,
for the data of 24 April 1996 and 30 June 1998, respectively.
7 = The combined flux of the WL20 triple system is listed here. See
Ressler & Barsony (2001AJ....121.1098R 2001AJ....121.1098R) for a thorough discussion of
this system. Individual source positions for each component are from
Barsony, Greene, & Blake (2002ApJ...572L..75B 2002ApJ...572L..75B).
8 = Our chop/nod directions and separations were poorly placed with respect
to the WL3, WL4, WL5, & GY244 asterism. Hence, we quote an upper limit
for WL5 derived from the average values for undetected sources for
24 April 1996, instead of measuring an upper limit directly from the
co-added data for this source.
Note (2): In general, the 12.5um fluxes were measured in a 0.72" aperture
(as per Table 1). The 12.5um flux was measured with a 0.7" and a 2"
aperture for 5 objects, WL12, WL22, GY292, IRS48, and GY352, in
columns F12.5um and F12.5-2, respectively. These observations were
obtained with LWS on Keck I on 29 June 1999.
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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- 13 A13 --- BKLT Source designations (G1)
14 A1 --- n_BKLT [p] primary
16 A1 --- f_BKLT Flag on BKLT (1)
18- 33 A16 --- OName Alias or other name
35- 36 A2 --- l_MIR [≤] Upper limit flag on MIR
37- 41 F5.3 Jy MIR ? The MIRLIN flux (2)
43- 48 F6.4 Jy e_MIR ? Uncertainty in MIR
50 A1 --- l_F10.8um Upper limit flag on F10.8um
51- 56 F6.3 Jy F10.8um ? ISOCAM 10.8µm flux
58- 62 F5.3 Jy e_F10.8um ? Uncertainty in F10.8um
64 A1 --- f_F10.8um Flag on F10.8um (1)
66- 70 F5.3 Jy LWS ? The LWS flux (12.5um)
72- 76 F5.3 Jy e_LWS ? Uncertainty in LWS
78- 82 F5.3 Jy F12.5um ? ISOCAM 12.5µm flux
84- 88 F5.3 Jy e_F12.5um ? Uncertainty in F12.5um
90 A1 --- f_F12.5um Flag on F12.5um (1)
92- 97 F6.3 Jy PGB1 ? Previous Ground-Based flux in MIR (N-band)
99-103 F5.3 Jy e_PGB1 ? Uncertainty in PGB1
105 A1 --- f_PGB1 Flag on PGB1 (1)
107-110 F4.2 Jy PGB2 ? Previous Ground-Based flux in MIR (N-band)
112-115 F4.2 Jy e_PGB2 ? Uncertainty in PGB2
117 A1 --- f_PGB2 Flag on PGB2 (1)
119-122 F4.2 Jy PGB3 ? Previous Ground-Based flux in MIR (N-band)
124-127 F4.2 Jy e_PGB3 ? Uncertainty in PGB3
129 A1 --- f_PGB3 Flag on PGB3 (1)
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Note (1): Flag, defined as follows:
1 = Flux from Table 2 of Wilking, Lada, & Young (1989ApJ...340..823W 1989ApJ...340..823W)
2 = Flux from Table 4 of Rydgren, Strom, & Strom (1976ApJS...30..307R 1976ApJS...30..307R)
3 = Flux from Table 1 of Lada & Wilking (1984ApJ...287..610L 1984ApJ...287..610L)
4 = Flux from Table 2 of Elias (1978ApJ...224..453E 1978ApJ...224..453E)
5 = Flux from Table 1 of Greene et al. (1994ApJ...434..614G 1994ApJ...434..614G)
6 = The SR24 system is a hierarchical triple, with a 6.0" separation
between the primary, SR24S (=BKLT J162658-244534), and the secondary,
SR24N (= BKLT J162658-244529), which itself consists of a 0.20"
separation binary. Although SR24S and SR24N were unresolved by ISOCAM,
previous ground-based observations did resolve these components.
N-band fluxes for SR24S are 0.78±0.029Jy (Wilking, Lada, & Young,
1989ApJ...340..823W 1989ApJ...340..823W) and 2.28±0.21Jy (Greene et al.,
1994ApJ...434..614G 1994ApJ...434..614G), to be compared with MIRLIN fluxes of 2.01Jy and
1.66Jy for SR24S on 26 June 1997 and 7 June 1998, respectively. N-band
fluxes for SR24N are 1.17±0.029 Jy (Wilking, Lada, & Young,
1989ApJ...340..823W 1989ApJ...340..823W) and 1.67±0.16Jy (Greene et al.,
1994ApJ...434..614G 1994ApJ...434..614G), to be compared with the MIRLIN flux of 1.40Jy for
both dates of observation. Therefore, we can conclude that it is the
single, primary star in this system, SR24S, which is the mid-infrared
variable.
7 = WL20 (= BKLT J162715-243843) is a triple system, which was noted as
highly variable in unresolved ISOCAM 6.7µm measurements. The
previously published N-band flux for the WL20 system from ground-based
measurements was 0.180±0.03Jy (Lada & Wilking, 1984ApJ...287..610L 1984ApJ...287..610L).
Our observations resolve the triple system in the mid-infrared, and show
that it is the "infrared companion", WL20S, which is the mid-infrared
variable (see Table 2).
8 = ISOCAM data from Wilking et al. (2001ApJ...551..357W 2001ApJ...551..357W).
Note (2): There is a second observation of WLY64 of 0.48±0.005.
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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- 13 A13 --- BKLT Source designations (G1)
15- 40 A26 --- OName Alias or other name
42 A1 --- f_OName Flag on OName (1)
44- 48 F5.2 mag Kmag ? The K band magnitude
50- 51 A2 --- l_H-K [≥ ] Lower limit flag on H-K
52- 55 F4.2 mag H-K ? The (H-K) color index
57- 58 A2 --- l_Sp+Index [≤] Upper limit flag on Sp+Index
59- 63 F5.2 --- Sp+Index ? The IR spectral index (2)
65- 70 A6 --- SED Spectral energy distribution class (4)
72-102 A31 --- rK Spectroscopically determined K-band veiling
and source (3)
104-132 A29 mag AV The V band extinction and source (3)
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Note (1): Flag on OName, defined as follows:
3 = The nature of WLY64 remains to be clarified, although it is listed as
an FU Ori candidate source by Luhman & Rieke, 1999ApJ...525..440L 1999ApJ...525..440L.
4 = Spectroscopically determined background giant (Luhman & Rieke,
1999ApJ...525..440L 1999ApJ...525..440L);
Note (2): Calculated between 2.2µm and either 10.8µm or 12.5µm, as
available from Table 2.
Note (3): From Luhman & Rieke (1999ApJ...525..440), unless otherwise indicated.
B02 = Boogert et al. (2002ApJ...570..708B 2002ApJ...570..708B);
BA92 = Bouvier & Appenzeller (1992A&AS...92..481B 1992A&AS...92..481B);
BGB02 = Barsony, Greene, & Blake (2002ApJ...572L..75B 2002ApJ...572L..75B);
DJW03 = Doppmann, Jaffe, & White (2003AJ....126.3043D 2003AJ....126.3043D);
D04 = Doppmann (2004, private communication);
GL97 = Greene & Lada (1997AJ....114.2157G 1997AJ....114.2157G);
GL02 = Greene & Lada (2002AJ....124.2185G 2002AJ....124.2185G);
GM95 = Greene & Meyer (1995ApJ...450..233G 1995ApJ...450..233G);
PGS03 = Prato, Greene, & Simon (2003ApJ...584..853P 2003ApJ...584..853P);
W94 = Walter et al. (1994AJ....107..692W 1994AJ....107..692W);
W01 = Wilking et al. (2001ApJ...551..357W 2001ApJ...551..357W);
WGM99 = Wilking, Greene, & Meyer (1999AJ....117..469W 1999AJ....117..469W)
Note (4): F.S. = flat spectrum. The SED class indicates an importance of
circumstellar matter, interpreted as an evolutionary sequence:
-- Class I object is one in which the central YSO has attained its
initial main-sequence mass but is still surrounded by a remnant
infall envelope and accretion disk;
-- Class II object is surrounded by an accretion disk;
-- Class III object has only a remnant, or absent, accretion disk.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- BKLT Source designations (G1)
15- 26 A12 --- OName Alias or other name
28- 29 I2 h RAh ? Hour of Right Ascension (J2000)
31- 32 I2 min RAm ? Minute of Right Ascension (J2000)
34- 38 F5.2 s RAs ? Second of Right Ascension (J2000)
40 A1 --- DE- Sign of the Declination (J2000)
41- 42 I2 deg DEd ? Degree of Declination (J2000)
44- 45 I2 arcmin DEm ? Arcminute of Declination (J2000)
47- 50 F4.1 arcsec DEs ? Arcsecond of Declination (J2000)
52- 56 A5 --- Type Multiplicity type (1)
58- 63 F6.3 arcsec Sep ? Separation (2)
65- 69 F5.1 deg PA ? Position angle (3)
71 A1 --- Res? Resolved in Mid-IR?
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Note (1): System type, defined as follows:
B = Binary;
SpB = Spectroscopic Binary;
T = Triple;
Q = Quadruple.
Note (2): The WL20W, WL20S, and WL20E separations are measured
E-W, S-W, and S-E. The uncertainties in IRS 2 and VSSG 27 are
both ±0.03.
Note (3): PAs are E of N, measured from the primary at K, except for IRS34,
where the primary is at N, since no resolved K band data exist.
The uncertainty in the IRS 2 and VSSG 27 PA's are ±4 and
±1, respectively.
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Global notes:
Note (G1): From Barsony et al. (1997, Cat. J/ApJS/112/109).
BKLT JHHMMSS+DDMMSS in Simbad.
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History:
* 04-Jan-2006: From electronic version of the journal
* 07-Aug-2007:
BKLT 162623-242603 transformed into BKLT 162623-244311 (tables 2 and )
BKLT 162730-242755 transformed into BKLT 162730-242744 (table4)
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 04-Jan-2006