J/MNRAS/532/424 Magellan/FIRE quasar [OIII] spectra (Temple+, 2024)
[O III] emission in z=2 quasars with and without broad absorption lines.
Temple M.J., Rankine A.L., Banerji M., Hennawi J.F., Hewett P.C.,
Matthews J.H., Nanni R., Ricci C., Richards G.T.
<Mon. Not. R. Astron. Soc. 532, 424 (2024)>
=2024MNRAS.532..424T 2024MNRAS.532..424T (SIMBAD/NED BibCode)
ADC_Keywords: QSOs; Spectra, infrared
Keywords: quasars: absorption lines - quasars: emission lines
Abstract:
Understanding the links between different phases of outflows from
active galactic nuclei is a key goal in extragalactic astrophysics.
Here, we compare [OIII] λλ 4960, 5008 outflow signatures
in quasars with and without broad absorption lines (BALs), aiming to
test how the broad absorption troughs seen in the rest-frame
ultraviolet are linked to the narrow line region outflows seen in the
rest-frame optical. We present new near-infrared spectra from
Magellan/FIRE that cover [OIII] in 12 quasars with 2.1<z<2.3 ,
selected to have strong outflow signatures in CIV λ 1550.
Combining with data from the literature, we build a sample of 73 BAL,
115 miniBAL, and 125 non-BAL quasars with 1.5<z<2.6. The strength and
velocity width of [OIII] correlate strongly with the C IV emission
properties, but no significant difference is seen in the [OIII]
emission-line properties between the BALs, non-BALs, and miniBALs once
the dependence on CIV emission is taken into account.
A weak correlation is observed between the velocities of CIV BALs and
[OIII] emission, which is accounted for by the fact that both outflow
signatures correlate with the underlying CIV emission properties. Our
results add to the growing evidence that BALs and non-BALs are drawn
from the same parent population and are consistent with a scenario
wherein BAL troughs are intermittent tracers of persistent quasar
outflows, with a part of such outflow becoming optically thick along
our line of sight for sporadic periods of time within which BALs are
observed.
Description:
We present near-infrared JHK spectra from Magellan/FIRE for twelve
quasars with 2.1<z<2.4, where Hbeta + [OIII] is observed in the H band
and Halpha in the K band. Data were gathered under CNTAC program
CN2020B-4 (PI: Temple).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 80 12 Source identification for new spectra
sp/* . 22 Spectra in ascii
fits/* . 22 Spectra in fits
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 19 A19 --- Name SDSS source name (JHHMMSS.ss+DDMMSS.s)
21- 39 F19.15 deg RAdeg Right ascension (J2000)
41- 60 F20.16 deg DEdeg Declination (J2000)
62- 68 F7.5 --- z Redshift
70- 80 A11 --- FileName Name of the spectrum file in subdirectory fits
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Byte-by-byte Description of file: sp/*
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Bytes Format Units Label Explanations
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3- 24 E22.17 0.1nm lambda Wavelength array (Angstroms in
vacuum), weighted by pixel
contributions
28- 49 E22.17 0.1nm lambdaGridMid Wavelength (Angstroms in vacuum)
evaluated at the bin centers of a
grid that is uniformly spaced in
log10-lambda/velocity
52- 74 E23.17 10-19W/m2/nm Flux Flux array in units of
10-17erg/s/cm2/Angstrom
78- 99 E22.17 10-19W/m2/nm ivar Inverse Variance array in units of
10-17erg/s/cm2/Angstrom
120 I1 --- mask [0/1] Mask array (1=Good,0=Bad)
124-145 E22.17 10-19W/m2/nm Telluric Telluric model
149-170 E22.17 10-19W/m2/nm ObjModel Object model for telluric correction
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Acknowledgements:
Matthew Temple, matthew.j.temple(at)durham.ac.uk
(End) Patricia Vannier [CDS] 11-Jul-2024