J/ApJS/147/305 IUE atlas of pre-main-sequence stars (Valenti+, 2003)
An IUE atlas of pre-main-sequence stars.
III. Co-added final archive spectra from the long-wavelength cameras.
Valenti J.A., Fallon A.A., Johns-Krull C.M.
<Astrophys. J. Suppl. Ser. 147, 305 (2003)>
=2003ApJS..147..305V 2003ApJS..147..305V
ADC_Keywords: Stars, pre-main sequence ; Spectra, ultraviolet
Mission_Name: IUE
Keywords: accretion, accretion disks - atlases - stars: pre-main-sequence -
ultraviolet: stars
Abstract:
We identified 137 T Tauri stars (TTS) and 97 Herbig Ae/Be (HAEBE)
stars observed by IUE in the wavelength interval 1900-3200Å. Each
low-resolution (R∼6Å) spectrum was visually inspected for source
contamination and data quality, and then all usable spectra were
combined to form a single time averaged spectrum for each star. For
sources with multiple observations, we characterized variability and
compared with previously published amplitudes at shorter wavelengths.
We combined several co-added spectra of diskless TTS to produce a pair
of intrinsic stellar spectra unaffected by accretion. We then fitted
spectra of TTS with the reddened sum of an intrinsic spectrum and a
schematic veiling continuum, measuring emission line fluxes from the
residuals. We used extinction and distance estimates from the
literature to convert measured Mg II line fluxes into intrinsic line
luminosities, noting that the IUE detection limit introduces a sample
bias such that intrinsic line luminosity is correlated with
extinction. This sample bias complicates any physical interpretation
of TTS intrinsic luminosities. We measured extinction toward HAEBE
stars by fitting our co-added IUE spectra with reddened spectra of
main-sequence stars and also from V band minus 3000Å color excess.
We measured excess line emission and absorption in spectra of HAEBE
stars divided by fitted spectra of main-sequence stars, noting that
HAEBE stars with an infrared excess indicating circumstellar material
typically also have anomalous UV line strengths. In the latter
situation, Mg II is usually shallower than in a main-sequence star of
the same spectral class, whereas Fe II lines are equally likely to be
deeper or shallower. Our co-added spectra of TTS, HAEBE stars, and
main-sequence templates are available electronically, in FITS and
ASCCI format, at
http://archive.stsci.edu/prepds/iuepms/ .
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 73 238 Pre-main-sequence stars observed by IUE with
LW cameras
table2.dat 76 22 Additional classifications from the literature
refs.dat 68 17 References
table3.dat 44 126 Measured Flux Variations
table6.dat 139 107 Measured Fluxes for TTS
table7.dat 28 32 Main-sequence template stars
table9.dat 87 97 Continuum Fluxes and Excess Line Emission
for HAEBE Stars
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See also:
http://archive.stsci.edu/prepds/iuepms/ :
IUE Spectral Atlas of Pre-Main-Sequence Stars
VI/110 : Final Merged Log of IUE Observations (NASA-ESA, 2000)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Internal identification number
4 A1 --- u_Seq [)] ) if none of the LW spectra are useful
6- 8 I3 --- VJL ? Identification number from Paper I,
Valenti et al., 2000ApJS..129..399V 2000ApJS..129..399V
9 A1 --- u_VJL [)] ) if none of the SW spectra are useful
11- 13 I3 --- HBC ? Number of Herbig & Bell, 1988LicOB1111....1H 1988LicOB1111....1H
15- 29 A15 --- Name Name of source
31- 46 A16 --- OName Other name
48- 60 A13 --- SpType Spectral type (1)
62- 67 A6 --- Cat PMS category
68 A1 --- n_Cat [h] Note on Cat (2)
70- 71 I2 --- N Number of useful IUE LW spectra
73 A1 --- sp [-] when there is no spectrum associated.
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Note (1): Spectral types preferentially from Herbig & Bell (1988LicOB1111....1H 1988LicOB1111....1H)
for TTS and The et al. (1994, Cat. J/A+AS/104/315 for HAEBE stars.
Note (2): h: We analyze as a CTTS, despite a HAEBE classification by
Gregorio-Hetem et al. (1992AJ....103..549G 1992AJ....103..549G).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Internal identification number
5- 17 A13 --- Name Name of source
19- 24 A6 --- Cat PMS category
25 A1 --- n_Cat [b] Note on Cat (1)
27- 28 I2 --- r_Cat References, in refs.dat file
30- 76 A47 --- Reasons Reasons of the classification
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Note (1): b: Status is uncertain as Hillenbrand et al. (1998,
Cat. J/AJ/116/1816 detect weak emission in the Ca II 8542Å line,
possibly indicating accretion.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number
4- 22 A19 --- BibCode BibCode
24- 44 A21 --- Aut Author's name
48- 78 A31 --- Com Comments
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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- 3 I3 --- Seq Identification number
5- 16 A12 --- Name Name
18- 22 A5 --- Cat PMS category
24- 25 I2 --- N Number of good IUE spectra used in analysis.
27- 33 F7.1 --- chi2r χ2r value
35 A1 --- l_Amp Limit flag on Amp
36- 39 F4.1 % Amp Relative amplitude of fluctuation
41- 44 F4.1 % e_Amp rms uncertainty on Amp
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Identification number
5 A1 --- l_ct2257 Upper limit flag on ct2257 (1)
6- 13 F8.4 [10mW/m2/nm] ct2257 Log of the continuum flux
near 2257Å (2)
15- 20 F6.4 [10mW/m2/nm] e_ct2257 ? Error in ct2257 (2)
22- 29 F8.4 [10mW/m2/nm] ct3060 Log of the continuum flux
near 3060Å (2)
31- 36 F6.4 [10mW/m2/nm] e_ct3060 Error in ct3060 (2)
38 A1 --- l_CII2330 Upper limit flag on CII2330 (1)
39- 44 F6.3 10-16W/m2 CII2330 Integrated C II (2330) line flux (3)
46- 50 F5.3 10-16W/m2 e_CII2330 ? Error in CII2330 (3)
52 A1 --- l_FeII2392 Upper limit flag on FeII2392 (1)
53- 59 F7.3 10-16W/m2 FeII2392 Integrated Fe II (2392) line flux (3)
61- 65 F5.3 10-16W/m2 e_FeII2392 ? Error in FeII2392 (3)
67 A1 --- l_FeII2508 Upper limit flag on FeII2508 (1)
68- 73 F6.3 10-16W/m2 FeII2508 Integrated Fe II (2508) line flux (3)
75- 79 F5.3 10-16W/m2 e_FeII2508 ? Error in FeII2508 (3)
81 A1 --- l_FeII2600 Upper limit flag on FeII2600 (1)
82- 88 F7.3 10-16W/m2 FeII2600 Integrated Fe II (2600) line flux (3)
90- 94 F5.3 10-16W/m2 e_FeII2600 ? Error in FeII2600 (3)
96 A1 --- l_FeII2742 Upper limit flag on FeII2742 (1)
97-102 F6.3 10-16W/m2 FeII2742 Integrated Fe II (2742) line flux (3)
104-108 F5.3 10-16W/m2 e_FeII2742 ? Error in FeII2742 (3)
110 A1 --- l_MgII2798 Upper limit flag on MgII2798 (1)
111-117 F7.3 10-16W/m2 MgII2798 Integrated Mg II (2798) line flux (3)
119-123 F5.3 10-16W/m2 e_MgII2798 ? Error in MgII2798 (3)
125 A1 --- l_FeII2995 Upper limit flag on FeII2995 (1)
126-132 F7.3 10-16W/m2 FeII2995 Integrated Fe II (2995) line flux (3)
134-138 F5.3 10-16W/m2 e_FeII2995 ? Error in FeII2995 (3)
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Note (1): Tabulated upper limits are twice the measured uncertainty.
Note (2): In units of erg/s/cm2/Å.
Note (3): In units of 10-13erg/s/cm2. Line fluxes in several columns
include significant contributions from more than one species.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HD HD number
9- 13 A5 --- SpType MK Spectral type
14- 16 I3 --- N Number of IUE spectra
18- 22 F5.2 mag AV Visual extinction
(from Neckel et al., 1980, Cat. II/62
24- 28 F5.2 mag (3000-V) Dereddened (3000-V) colour index
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Identification number
5 A1 --- l_ct2257 Upper limit flag on ct2257 (1)
6- 13 F8.4 [10mW/m2/nm] ct2257 Log of the continuum flux
near 2257Å (2)
15- 20 F6.4 [10mW/m2/nm] e_ct2257 ? Error in ct2257 (2)
22- 29 F8.4 [10mW/m2/nm] ct3060 Log of the continuum flux
near 3060Å (2)
31- 36 F6.4 [10mW/m2/nm] e_ct3060 Error in ct3060 (2)
38 A1 --- l_FeII2392 Upper limit flag on FeII2392 (1)
39- 43 F5.2 10-16W/m2 FeII2392 ? Integrated Fe II (2392) line flux (3)
45- 48 F4.2 10-16W/m2 e_FeII2392 ? Error in FeII2392 (3)
50 A1 --- l_FeII2600 Upper limit flag on FeII2600 (1)
51- 55 F5.2 10-16W/m2 FeII2600 ? Integrated Fe II (2600) line flux (3)
57- 60 F4.2 10-16W/m2 e_FeII2600 ? Error in FeII2600 (3)
61 A1 --- u_FeII2600 [:] Uncertainty flag on FeII2600
63 A1 --- l_FeII2742 Upper limit flag on FeII2742 (1)
64- 68 F5.2 10-16W/m2 FeII2742 ? Integrated Fe II (2742) line flux (3)
70- 73 F4.2 10-16W/m2 e_FeII2742 ? Error in FeII2742 (3)
74 A1 --- u_FeII2742 [:] Uncertainty flag on FeII2742
76 A1 --- l_MgII2798 Upper limit flag on MgII2798 (1)
77- 81 F5.2 10-16W/m2 MgII2798 ? Integrated Mg II (2798) line flux (3)
83- 86 F4.2 10-16W/m2 e_MgII2798 ? Error in MgII2798 (3)
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Note (1): Tabulated upper limits are twice the measured uncertainty.
Note (2): In units of erg/s/cm2/Angstrom.
Note (3): In units of 10-13 erg/s/cm2. Line fluxes in several columns
include significant contributions from more than one species.
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History:
From electronic version of the journal
References:
Valenti et al., Paper I 2000ApJS..129..399V 2000ApJS..129..399V
Johns-Krull et al., Paper II 2000ApJ...539..815J 2000ApJ...539..815J
(End) Greg Schwarz [AAS], Patricia Bauer [CDS] 22-Sep-2003