J/ApJS/150/165 AGNs emission-line from Post-COSTAR (Kuraszkiewicz+, 2004)
Emission line properties of active galactic nuclei from a Post-COSTAR Hubble
Space Telescope Faint Object Spectrograph spectral atlas.
Kuraszkiewicz J.K., Green P.J., Crenshaw D.M., Dunn J., Forster K.,
Vestergaard M., Aldcroft T.L.
<Astrophys. J. Suppl. Ser., 150, 165 (2004)>
=2004ApJS..150..165K 2004ApJS..150..165K
ADC_Keywords: Atlases ; Active gal. nuclei ; QSOs ; Spectra, ultraviolet
Keywords: atlases - galaxies: active - quasars: emission lines -
quasars: general - ultraviolet: galaxies
Abstract:
We present consistent emission-line measurements for active galactic
nuclei (AGNs), useful for reliable statistical studies of emission
line properties. This paper joins a series including similar
measurements of 993 spectra from the Large Bright Quasar Survey and
174 spectra of AGNs obtained from the Faint Object Spectrograph (FOS)
on the Hubble Space Telescope (HST) prior to the installation of
COSTAR. This time we concentrate on 220 spectra obtained with the
FOS after the installation of COSTAR, completing the emission line
analysis of all FOS archival spectra. We use the same automated
technique as in previous papers, which accounts for Galactic
extinction, models blended optical and UV iron emission, includes
Galactic and intrinsic absorption lines, and models emission lines
using multiple Gaussians. We present UV and optical emission line
parameters (equivalent widths, fluxes, FWHM, and line positions) for
a large number (28) of emission lines including upper limits for
undetected lines. Further scientific analyses will be presented in
subsequent papers.
Description:
The sample was assembled by cross-correlating the Veron-Cetty & Veron
(1996ESOSR..17....1V 1996ESOSR..17....1V, Cat. VII/188, 7th Edition) catalog of AGNs
with the MAST (Multimission Archive at Space Telescope) holdings.
BL Lac objects were ignored, as their spectra show no emission lines.
Starburst galaxies and broad absorption line (BAL) quasars (where
emission lines are heavily disrupted by absorption features) were not
included. We chose all available (UV and optical) spectrophotometric
archival data that have been observed with the Faint Object
Spectrograph (FOS) on HST after the installation of COSTAR (i.e.,
after 1993 December). FOS spectra obtained prior to 1993 December
have been analyzed by us in Paper II (Kuraszkiewicz et al., 2002,
Cat. J/ApJS/143/257).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 58 220 List of objects and spectra
table2.dat 57 707 Representative list of objects and FOS spectra
table3.dat 76 220 Continuum parameters
table4a.dat 135 9460 Emission line measurements
table4b.dat 155 220 Total line FWHM measurements
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See also:
J/ApJS/143/257 : AGN emission line properties (Kuraszkiewicz+, 2002)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Object designation (1)
10 A1 --- f_Name [*] BL Lac object, see note (2)
12- 25 A14 --- CName Common name
27- 31 A5 --- Type AGN type (3)
33- 37 F5.3 --- z Redshift
40- 44 F5.2 10+20cm-2 NH Neutral hydrogen column density
46- 56 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): We include this BL Lac object as it shows weak emission lines.
Note (3): AGN types are as follows:
Q = QSO;
Sy1 = Seyfert 1;
Sy2 = Seyfert 2;
NLS1 = Narrow Line Seyfert 1;
NLRG = Narrow Line Radio Galaxy.
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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- 11 A11 --- NSpect Spectrum name (G1)
14- 22 A9 --- Dataset HST Dataset
26- 27 A2 --- Config FOC configuration
30- 34 A5 --- Grating Grating
37- 43 F7.1 s Exp Exposure time
47- 57 A11 "MMM-DD-YYYY" Time Date of observation
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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- 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 2σ error in GammaUV
25- 29 F5.2 --- e_GammaUV ? Lower 2σ error in GammaUV
31- 36 F6.3 10-16W/m2/nm F(norm) Normalization of UV power law in units of
10-14erg/cm2/s/Å (2)
38- 42 F5.3 10-16W/m2/nm E_F(norm) Upper 2σ error in F(norm)
44- 48 F5.3 10-16W/m2/nm e_F(norm) Lower 2σ error in F(norm)
50- 55 F6.1 0.1nm WLnorm Observed norm wavelength in Angstroems
57- 61 F5.2 --- GammaOpt ? Optical power law continuum slope (2)
63- 68 F6.2 --- E_GammaOpt ? Upper 2σ error in GammaOpt
70- 74 F5.2 --- e_GammaOpt ? Lower 2σ error in GammaOpt
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Note (2): The dereddened continuum spectrum is fitted as
F(λ) = F(norm) . λ-GammaUV
for UV wavelengths (λrest<4200Å), and
F(λ) = F(norm) . λ-GammaOpt.
for optical wavelengths (λrest>4200Å).
Slopes with no listed errors show the assumed slope value in cases
where only a single continuum window was available.
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Byte-by-byte Description of file: table4a.dat
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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 2σ error limit on FWHM
53- 57 I5 km/s e_FWHM Lower 2σ error limit on FWHM
60- 64 I5 km/s VPeak Gaussian emission line model peak offset from
expected position based on tabulated redshift
67- 71 I5 km/s E_VPeak Upper 2σ error limit on VPeak
73- 77 I5 km/s e_VPeak Lower 2σ error limit on VPeak
80- 86 F7.2 0.1nm EW Rest frame equivalent width in Angstroms
90- 95 F6.2 0.1nm E_EW Upper 2σ error limit on EW (2)
98-103 F6.2 0.1nm e_EW Lower 2σ error limit on EW (2)
106-112 F7.2 10-17W/m2 Flux Observed flux in units of 10-14erg/s/cm2
116-121 F6.2 10-17W/m2 E_Flux Upper 2σ error limit on Flux (2)
124-129 F6.2 10-17W/m2 e_Flux Lower 2σ error limit on Flux (2)
131-132 I2 --- o_Line ? Number of narrow absorption features
used in the emission line modeling
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Note (2): 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, J/ApJS/143/257) with no associated errors.
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Byte-by-byte Description of file: table4b.dat
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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 Lya ?=0 Rest frame FWHM of total Lyα
22- 27 I6 km/s E_Lya ?=0 Upper 2σ error limit on Lya
30- 35 I6 km/s e_Lya ?=0 Lower 2σ error limit on Lya
38- 43 I6 km/s CIV ?=0 Rest frame FWHM of total CIV
46- 51 I6 km/s E_CIV ?=0 Upper 2σ error limit on CIV
54- 59 I6 km/s e_CIV ?=0 Lower 2σ error limit on CIV
62- 67 I6 km/s CIII ?=0 Rest frame FWHM of total CIII]
70- 75 I6 km/s E_CIII ?=0 Upper 2σ error limit on CIII
78- 83 I6 km/s e_CIII ?=0 Lower 2σ error limit on CIII
86- 91 I6 km/s MgII ?=0 Rest frame FWHM of total MgII
94- 99 I6 km/s E_MgII ?=0 Upper 2σ error limit on MgII
102-107 I6 km/s e_MgII ?=0 Lower 2σ error limit on MgII
110-115 I6 km/s Hb ?=0 Rest frame FWHM of total Hβ
118-123 I6 km/s E_Hb ?=0 Upper 2σ error limit on Hb
126-131 I6 km/s e_Hb ?=0 Lower 2σ error limit on Hb
134-139 I6 km/s Ha ?=0 Rest frame FWHM of total Hα
142-147 I6 km/s E_Ha ?=0 Upper 2σ error limit on Ha
150-155 I6 km/s e_Ha ?=0 Lower 2σ error limit on Ha
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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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History:
From electronic version of the journal
* 04-Dec-2004: a few modifications in the columns "NSpect" done at CDS:
0853+5118oa turned into 0853+5118oc (table1 & table2)
2156+7222oa turned into 2156+0722oa (table3)
1017-2046oa and 1017-2046ob turned into 1017-2046oA and 1017-2046oB
(tables 4)
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 30-Jan-2004