Документ взят из кэша поисковой машины. Адрес оригинального документа : http://hea-www.harvard.edu/~pgreen/Papers/postcos.tablenotes Дата изменения: Mon Sep 15 22:14:47 2003 Дата индексирования: Tue Oct 2 02:32:35 2012 Кодировка: Поисковые слова: meteor

Files Summary:


table1_electronic List of the 180 objects and spectra
table2_electronic List of grating and datasets used
table3_electronic Continuum parameters
table4_electronic Emission line measurements
table4b_electronic Total line FWHM measurements



Byte-by-byte Description of file: table1_electronic
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Object designation (1)
10 A1 f_Name [*] See note (3)
12- 25 A14 --- CName Common name
27- 31 A5 --- Type AGN type (2)
33- 37 F5.3 --- z Redshift
39- 43 F6.2 10+20/cm2 NH Neutral hydrogen column density
45- 55 A11 --- NSpect Spectrum name (G1)
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Note (1):Based on the equinox J2000 position (in standard IAU format consisting
of HHMM+/-DDMM).
Note (2): AGN type:
Q = QSO
Sy1 = Seyfert 1
Sy2 = Seyfert 2
NLS1 = Narrow Line Seyfert 1
NLRG = Narrow Line Radio Galaxy
Note (3): We include this BL Lac object as it shows weak emission lines.
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Byte-by-byte Description of file: table2_electronic
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Bytes Format Units Label Explanations
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1- 11 A11 --- NSpect Spectrum name (G1)
14- 22 A9 --- Dataset HST Dataset
26- 27 A2 --- Config Detector used
30- 34 A5 --- Grating Grating
37- 43 F7.1 sec Exp Exposure time
47- 57 A11 --- Time Time of observation
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Byte-by-byte Description of file: table3_electronic
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Bytes Format Units Label Explanations
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1- 11 A11 --- Nspect Spectrum name (G1)
12 A1 --- f_Nspect [*] See notes on spectra in Appendix
14- 18 F5.2 --- GammaUV UV power law continuum slope (2)
20- 23 F4.2 --- E_GammaUV ? Upper 2{sigma} error in GammaUV
25- 29 F5.2 --- e_GammaUV ? Lower 2{sigma} error in GammaUV
31- 36 F6.3 10-13mW/m2/nm Norm Normalization of UV power law in units
of 10^-14^erg/cm^2^/s/Angstroems
38- 42 F5.3 10-13mW/m2/nm E_Norm Upper 2{sigma} error in Norm
44- 48 F5.3 10-13mW/m2/nm e_Norm Lower 2{sigma} error in Norm
50- 55 F6.1 0.1nm Wave Observed wavelength in Angstroems
57- 61 F5.2 --- GammaOpt ? Optical power law continuum slope (3)
63- 68 F6.2 --- E_GammaOpt ? Upper 2{sigma} error in GammaOpt
70- 74 F5.2 --- e_GammaOpt ? Lower 2{sigma} error in GammaOpt
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Note (2): Defined as f_{lambda}_ {prop to} {lambda}^-GammaUV^.
GammaUV is fitted at {lambda}_rest_<4200{AA}. Slopes with no listed
errors show the assumed slope value in cases where only a single
continuum window was available.
Note (3): Defined as f_{lambda}_ {prop to} {lambda}^-GammaOpt^.
GammaOpt is fitted at {lambda}_rest_>4200{AA}.
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Byte-by-byte Description of file: table4_electronic
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Bytes Format Units Label Explanations
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1- 11 A11 --- NSpect Spectrum name (G1)
13- 20 F8.5 --- z Redshift
22- 38 A17 --- Line Emission line identification
40- 44 I5 km/s FWHM Rest frame Full Width at Half Maximum
47- 51 I5 km/s E_FWHM Upper 2{sigma} error limit on FWHM
53- 58 I6 km/s e_FWHM Lower 2{sigma} error limit on FWHM
61- 65 I5 km/s VPeak Gaussian emission line model peak offset
from expected position based on tabulated
redshift
69- 72 I4 km/s E_VPeak Upper 2{sigma} error limit on VPeak
74- 79 I6 km/s e_VPeak Lower 2{sigma} error limit on VPeak
82- 88 F7.2 0.1nm EW Rest frame equivalent width in Angstroms
92- 97 F6.2 0.1nm E_EW Upper 2{sigma} error limit on EW (1)
100-106 F7.2 0.1nm e_EW Lower 2{sigma} error limit on EW (1)
109-115 F7.2 10-14mW/m2 Flux Observed flux in units of 10^-14^erg/s/cm^2^
119-124 F6.2 10-14mW/m2 E_Flux Upper 2{sigma} error limit on Flux (1)
127-133 F7.2 10-14mW/m2 e_Flux Lower 2{sigma} error limit on Flux (1)
135-136 I2 --- NAbs Number of narrow absorption features used
in the emission line modeling
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Note (1): Based on the uncertainties in the amplitude and FWHM of the Gaussian
model and do not include an error from an uncertainty in the
underlying continuum flux level which we estimate to be about 10%.
For emission lines where only an upper limit on Flux and EW is
available, no values for the VPeak are quoted as the position of the
line was fixed at the line's expected wavelength. Also, the FWHM
value in this case was set to the median value for the LBQS sample
(see Table 3, Paper~II) with no associated errors.
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Byte-by-byte Description of file: table4b_electronic
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Bytes Format Units Label Explanations
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1- 11 A11 --- NSpect Spectrum name (G1)

14- 19 I6 km/s FWHM_ly Rest frame Full Width at Half Maximum of total Lya
22- 27 I6 km/s E_FWHM Upper 2{sigma} error limit on FWHM of total Lya
30- 35 I6 km/s e_FWHM Lower 2{sigma} error limit on FWHM of total Lya

38- 43 I6 km/s FWHM_c4 Rest frame Full Width at Half Maximum of total CIV
46- 51 I6 km/s E_FWHM Upper 2{sigma} error limit on FWHM of total CIV
54- 59 I6 km/s e_FWHM Lower 2{sigma} error limit on FWHM of total CIV

62- 67 I6 km/s FWHM_c3 Rest frame Full Width at Half Maximum of total CIII]
70- 75 I6 km/s E_FWHM Upper 2{sigma} error limit on FWHM of total CIII]
78- 83 I6 km/s e_FWHM Lower 2{sigma} error limit on FWHM of total CIII]

86- 91 I6 km/s FWHM_mg Rest frame Full Width at Half Maximum of total MgII
94- 99 I6 km/s E_FWHM Upper 2{sigma} error limit on FWHM of total MgII
102-107 I6 km/s e_FWHM Lower 2{sigma} error limit on FWHM of total MgII

110-115 I6 km/s FWHM_hb Rest frame Full Width at Half Maximum of total Hbeta
118-123 I6 km/s E_FWHM Upper 2{sigma} error limit on FWHM of total Hbeta
126-131 I6 km/s e_FWHM Lower 2{sigma} error limit on FWHM of total Hbeta

134-139 I6 km/s FWHM_ha Rest frame Full Width at Half Maximum of total Halpha
142-147 I6 km/s E_FWHM Upper 2{sigma} error limit on FWHM of total Halpha
150-155 I6 km/s e_FWHM Lower 2{sigma} error limit on FWHM of total Halpha


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Global notes:
Note (G1):
Based on the equinox J2000 position (in standard IAU format
consisting of HHMM+/-DDMM). In addition to this, a two letter
designation is used for the spectra indicating that the spectra are
from a post-COSTAR observation (o) and whether there is
more than one spectrum of the same object (a-z). A capital
letter at the end of the name indicates that the object is
a gravitational lens and that separate spectra of each
lensed component were observed and analyzed.
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