J/MNRAS/540/562 Candidate super-Eddington quasars spectra (Buendia-Rios+, 2025)
Large Binocular Telescope infrared observations of candidate
super-Eddington quasars.
Buendia-Rios T.M., Marziani P., Negret C.A., Dultzin D.
<Mon. Not. R. Astron. Soc. 540, 562-581 (2025)>
=2025MNRAS.540..562B 2025MNRAS.540..562B (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Spectra, infrared
Keywords: line: formation - line: profiles - galaxies: nuclei -
quasars: emission lines - quasars: supermassive black holes
Abstract:
Quasars accreting at very high rates are believed to be prime movers
of galactic evolution because of their high radiative and mechanical
output. The study presented in this paper investigates a sample of six
highly accreting quasars at redshifts (z=2-3) using near-infrared
observations from the LUCI spectrograph at the Large Binocular
Telescope (LBT). The aim is obtain a precise measure of the quasar
systemic redshift and accretion parameters (black hole mass and
Eddington ratio) primarily from the Hβ line, and on second stance
from other intermediate and low ionization lines. Outflow dynamical
parameters (mass rate of outflowing gas, its kinetic power and
momentum rate) were estimated from the CIV emission line that is
perhaps the most easily accessible tracer of high-ionization winds
from the accretion disk, obtained from the Sloan Digital Sky Survey.
In addition, the joint analysis of the rest-frame optical and UV
spectra allowed us to estimate the chemical composition of the broad
line emitting gas. The high metal content of the outflowing gas
(Z≳10Z☉) and the high values of thrust and kinetic power may
induce a chemical feedback effect in the quasar host, in addition to
mechanical feedback.
Description:
We presented new LUCI observations at the LBT covering a
sample of 6 highly accreting quasars (super-Eddington candidates) at
z∼2. The NIR spectrographic camera LUCI allowed us to cover the
Hβ spectral region which yields a wealth of diagnostic
information on the physical condition and dynamics of the line
emitting region. SDSS spectra were used to analyze the spectral region
of the UV emission lines from SiIVλ1397+OIV]λ1402 to
MgIIλ2800.
IR spectra in ASCII format provided as individual files.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 151 6 Source identification and basic properties of
the LUCI-LBT sample
sp/* . 6 Individual spectra
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- SDSS SDSS coordinate name, JHHMMSS.ss+DDMMSS.s
21- 22 I2 h RAh Right ascension (J2000)
24- 25 I2 min RAm Right ascension (J2000)
27- 31 F5.2 s RAs Right ascension (J2000)
33 A1 --- DE- Declination sign (J2000)
34- 35 I2 deg DEd Declination (J2000)
37- 38 I2 arcmin DEm Declination (J2000)
40- 43 F4.1 arcsec DEs Declination (J2000)
45- 50 F6.3 mag Vmag Apparent V magnitude
52- 57 F6.3 mag imag SDSS magnitude in the i band
59- 64 F6.3 mag zmag SDSS magnitude in the g band
66- 71 F6.3 mag Hmag ?=- Apparent IR magnitude in the H-band
(2MASS) or lower value of Hmag interval
72 A1 --- --- [-]
73- 77 F5.2 mag Hmag2 ? Upper value of zmag interval
78 A1 --- n_Hmag2 [*] Note on Hmag and Hmag2 (1)
80- 86 F7.5 --- zsys Systemic redshift
88- 94 F7.5 --- e_zsys Redshift uncertainty
96- 99 F4.2 --- AM Airmass
101-139 A39 --- Class Quasar classification (2)
141-151 A11 --- FileName Name of the spectrum file in subdirectory sp
--------------------------------------------------------------------------------
Note (1): for J093403.96+315331.3, apparent magnitude in the H-band using our
LBT estimates.
Note (2): Quasar classification:
FBQS = first bright quasar survey
BAL = broad absorption lines
RE = radio emission detected in FIRST
RK = Kellermann's ratio (Kellermann et al., 1989AJ.....98.1195K 1989AJ.....98.1195K)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: sp/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 F11.6 0.1nm lambda Quasar rest-frame wavelength
17- 28 F12.6 10-19W/m2/nm Flux Specific flux at rest-frame,
in 10-17erg/s/cm2/Å
33- 42 F10.6 0.1nm FluxNoise ?=- Flux noise vector
--------------------------------------------------------------------------------
Acknowledgements:
Tania Buendia Rios, tbuendia(at)astro.unam.mx
References:
Almeida et al., 2023ApJS..267...44A 2023ApJS..267...44A,
Sloan Digital Sky Surveys (SDSS), Release 18 (DR18)
(End) Patricia Vannier [CDS] 01-May-2025