J/A+A/685/A25 Faint, unobscured quasars at z>6 (Andika+, 2024)
Tracing the rise of supermassive black holes. A panchromatic search for faint,
unobscured quasars at z ≳ 6 with COSMOS-Web and other surveys.
Andika I.T., Jahnke K., Onoue M., Silverman J.D., Fitriana I.K.,
Bongiorno A., Brinch M., Casey C.M., Faisst A., Gillman S., Gozaliasl G.,
Hayward C.C., Hirschmann M., Kocevski D., Koekemoer A.M., Kokorev V.,
Lambrides E., Lee M.M., Rich R.M., Trakhtenbrot B., Urry C.M.,
Wilkins S.M., Vijayan A.P.
<Astron. Astrophys. 685, A25 (2024)>
=2024A&A...685A..25A 2024A&A...685A..25A (SIMBAD/NED BibCode)
ADC_Keywords: Black holes ; QSOs ; Energy distributions ; Infrared ;
Optical
Keywords: methods: data analysis - methods: observational - galaxies: active -
galaxies: high-redshift - quasars: general -
quasars: supermassive black holes
Abstract:
We report the identification of 64 new candidates of compact galaxies,
potentially hosting faint quasars with bolometric luminosities of
Lbol=1043-1046erg/s, residing in the reionization epoch within the
redshift range of 6≲z≲8. These candidates were selected by
harnessing the rich multiband datasets provided by the emerging
JWST-driven extragalactic surveys, focusing on COSMOS-Web, as well as
JADES, UNCOVER, CEERS, and PRIMER. Our search strategy includes two
stages: applying stringent photometric cuts to catalog-level data and
detailed spectral energy distribution fitting. These techniques
effectively isolate the quasar candidates while mitigating
contamination from low-redshift interlopers, such as brown dwarfs and
nearby galaxies. The selected candidates indicate physical traits
compatible with low-luminosity active galactic nuclei, likely hosting
∼105-107M☉ supermassive black holes (SMBHs) living in
galaxies with stellar masses of ∼108-1010M☉. The SMBHs
selected in this study, on average, exhibit an elevated mass compared
to their hosts, with the mass ratio distribution slightly higher than
those of galaxies in the local Universe. As with other high-z studies,
this is at least in part due to the selection method for these
quasars. An extensive Monte Carlo analysis provides compelling
evidence that heavy black hole seeds from the direct collapse scenario
appear to be the preferred pathway to mature this specific subset of
SMBHs by z∼7. Notably, most of the selected candidates might have
emerged from seeds with masses of ∼105M☉, assuming a thin disk
accretion with an average Eddington ratio of fEdd=0.6±0.3 and a
radiative efficiency of epsilon=0.2±0.1. This work underscores the
significance of further spectroscopic observations, as the quasar
candidates presented here offer exceptional opportunities to delve
into the nature of the earliest galaxies and SMBHs that formed during
cosmic infancy.
Description:
Photometric properties and spectral energy distribution fitting
results for 350 compact galaxy candidates, including 64 quasar
candidates at z>6, are presented.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb1.dat 2573 350 Photometric properties and
spectral energy distributions
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Name (name)
12- 29 F18.14 deg RAdeg Right Ascension (J2000) (ra)
31- 48 F18.14 deg DEdeg Declination (J2000) (dec)
50- 68 F19.15 nJy e_FF090W ? Total flux error based on the
F090W photometry (e_f090w)
70- 88 F19.15 nJy e_FF105W ? Total flux error based on the
F105W photometry (e_f105w)
90- 107 F18.14 nJy e_FF110W ? Total flux error based on the
F110W photometry (e_f110w)
109- 126 F18.15 nJy e_FF115W Total flux error based on the
F115W photometry (e_f115w)
128- 146 F19.15 nJy e_FF125W ? Total flux error based on the
F125W photometry (e_f125w)
148- 165 F18.14 nJy e_FF140W ? Total flux error based on the
F140W photometry (e_f140w)
167- 184 F18.15 nJy e_FF150W Total flux error based on the
F150W photometry (e_f150w)
186- 205 F20.15 nJy e_FF160W ? Total flux error based on the
F160W photometry (e_f160w)
207- 227 F21.13 nJy e_FF1800W []? Total flux error based on the
F1800W photometry (e_f1800w)
229- 247 F19.15 nJy e_FF182M ? Total flux error based on the
F182M photometry (e_f182m)
249- 267 F19.15 nJy e_FF200W ? Total flux error based on the
F200W photometry (e_f200w)
269- 287 F19.15 nJy e_FF210M ? Total flux error based on the
F210M photometry (e_f210m)
289- 307 F19.15 nJy e_FF277W ? Total flux error based on the
F277W photometry (e_f277w)
309- 326 F18.15 nJy e_FF335M ? Total flux error based on the
F335M photometry (e_f335m)
328- 346 F19.15 nJy e_FF356W ? Total flux error based on the
F356W photometry (e_f356w)
348- 366 F19.15 nJy e_FF410M ? Total flux error based on the
F410M photometry (e_f410m)
368- 384 F17.14 nJy e_FF430M ? Total flux error based on the
F430M photometry (e_f430m)
386- 404 F19.15 nJy e_FF435W ? Total flux error based on the
F435W photometry (e_f435w)
406- 423 F18.15 nJy e_FF444W Total flux error based on the
F444W photometry (e_f444w)
425- 441 F17.14 nJy e_FF460M ? Total flux error based on the
F460M photometry (e_f460m)
443- 460 F18.14 nJy e_FF475W ? Total flux error based on the
F475W photometry (e_f475w)
462- 479 F18.14 nJy e_FF480M ? Total flux error based on the
F480M photometry (e_f480m)
481- 503 F23.15 nJy e_FF606W []? Total flux error based on the
F606W photometry (e_f606w)
505- 522 F18.13 nJy e_FF770W ? Total flux error based on the
F770W photometry (e_f770w)
524- 541 F18.15 nJy e_FF775W ? Total flux error based on the
F775W photometry (e_f775w)
543- 561 F19.15 nJy e_FF814W ? Total flux error based on the
F814W photometry (e_f814w)
563- 580 F18.14 nJy e_FF850LP ? Total flux error based on the
F850LP photometry (e_f850lp)
582- 598 F17.14 nJy e_FHSC-g ? Total flux error based on the
HSC-g photometry (e_hsc-g)
600- 616 F17.13 nJy e_FHSC-i ? Total flux error based on the
HSC-i photometry (e_hsc-i)
618- 635 F18.14 nJy e_FHSC-r ? Total flux error based on the
HSC-r photometry (e_hsc-r)
637- 653 F17.13 nJy e_FHSC-y ? Total flux error based on the
HSC-y photometry (e_hsc-y)
655- 671 F17.13 nJy e_FHSC-z ? Total flux error based on the
HSC-z photometry (e_hsc-z)
673- 689 F17.14 nJy e_FHST-F814W ? Total flux error based on the
HST-F814W photometry
(e_hst-f814w)
691- 707 F17.13 nJy e_FUVISTA-H ? Total flux error based on the
UVISTA-H photometry (e_uvista-h)
709- 725 F17.13 nJy e_FUVISTA-J ? Total flux error based on the
UVISTA-J photometry (e_uvista-j)
727- 743 F17.13 nJy e_FUVISTA-Ks ? Total flux error based on the
UVISTA-Ks photometry
(e_uvista-ks)
745- 760 F16.12 nJy e_FUVISTA-Y ? Total flux error based on the
UVISTA-Y photometry (e_uvista-y)
762- 781 F20.15 nJy FF090W ? Total flux based on the F090W
photometry (f_f090w)
783- 802 F20.15 nJy FF105W ? Total flux based on the F105W
photometry (f_f105w)
804- 820 F17.13 nJy FF110W ? Total flux based on the F110W
photometry (f_f110w)
822- 839 F18.14 nJy FF115W Total flux based on the F115W
photometry (f_f115w)
841- 859 F19.14 nJy FF125W ? Total flux based on the F125W
photometry (f_f125w)
861- 879 F19.14 nJy FF140W ? Total flux based on the F140W
photometry (f_f140w)
881- 899 F19.14 nJy FF150W Total flux based on the F150W
photometry (f_f150w)
901- 920 F20.15 nJy FF160W ? Total flux based on the F160W
photometry (f_f160w)
922- 939 F18.13 nJy FF1800W ? Total flux based on the F1800W
photometry (f_f1800w)
941- 955 E15.8 nJy FF182M ? Total flux based on the F182M
photometry (f_f182m)
957- 975 F19.14 nJy FF200W ? Total flux based on the F200W
photometry (f_f200w)
977- 991 E15.8 nJy FF210M ? Total flux based on the F210M
photometry (f_f210m)
993-1012 F20.14 nJy FF277W ? Total flux based on the F277W
photometry (f_f277w)
1014-1032 F19.14 nJy FF335M ? Total flux based on the F335M
photometry (f_f335m)
1034-1052 F19.14 nJy FF356W ? Total flux based on the F356W
photometry (f_f356w)
1054-1073 F20.14 nJy FF410M ? Total flux based on the F410M
photometry (f_f410m)
1075-1092 F18.14 nJy FF430M ? Total flux based on the F430M
photometry (f_f430m)
1094-1113 F20.16 nJy FF435W ? Total flux based on the F435W
photometry (f_f435w)
1115-1133 F19.14 nJy FF444W Total flux based on the F444W
photometry (f_f444w)
1135-1152 F18.13 nJy FF460M ? Total flux based on the F460M
photometry (f_f460m)
1154-1172 F19.15 nJy FF475W ? Total flux based on the F475W
photometry (f_f475w)
1174-1192 F19.14 nJy FF480M ? Total flux based on the F480M
photometry (f_f480m)
1194-1213 F20.16 nJy FF606W ? Total flux based on the F606W
photometry (f_f606w)
1215-1234 F20.14 nJy FF770W ? Total flux based on the F770W
photometry (f_f770w)
1236-1254 F19.15 nJy FF775W ? Total flux based on the F775W
photometry (f_f775w)
1256-1275 F20.16 nJy FF814W ? Total flux based on the F814W
photometry (f_f814w)
1277-1295 F19.15 nJy FF850LP ? Total flux based on the F850LP
photometry (f_f850lp)
1297-1315 F19.16 nJy FHSC-g ? Total flux based on the HSC-g
photometry (f_hsc-g)
1317-1336 F20.16 nJy FHSC-i ? Total flux based on the HSC-i
photometry (f_hsc-i)
1338-1357 F20.16 nJy FHSC-r ? Total flux based on the HSC-r
photometry (f_hsc-r)
1359-1379 F21.16 nJy FHSC-y ? Total flux based on the HSC-y
photometry (f_hsc-y)
1381-1401 F21.16 nJy FHSC-z ? Total flux based on the HSC-z
photometry (f_hsc-z)
1403-1423 F21.16 nJy FHST-F814W ? Total flux based on the
HST-F814W photometry
(f_hst-f814w)
1425-1443 F19.13 nJy FUVISTA-H ? Total flux based on the
UVISTA-H photometry (f_uvista-h)
1445-1462 F18.13 nJy FUVISTA-J ? Total flux based on the
UVISTA-J photometry (f_uvista-j)
1464-1482 F19.13 nJy FUVISTA-Ks ? Total flux based on the
UVISTA-Ks photometry
(f_uvista-ks)
1484-1504 F21.16 nJy FUVISTA-Y ? Total flux based on the
UVISTA-Y photometry (f_uvista-y)
1506-1525 F20.16 --- SNRF090W ? Signal-to-noise ratio based on
the F090W photometry (snr_f090w)
1527-1546 F20.16 --- SNRF105W ? Signal-to-noise ratio based on
the F105W photometry (snr_f105w)
1548-1564 F17.14 --- SNRF110W ? Signal-to-noise ratio based on
the F110W photometry (snr_f110w)
1566-1582 F17.14 --- SNRF115W Signal-to-noise ratio based on the
F115W photometry (snr_f115w)
1584-1602 F19.15 --- SNRF125W ? Signal-to-noise ratio based on
the F125W photometry (snr_f125w)
1604-1623 F20.16 --- SNRF140W ? Signal-to-noise ratio based on
the F140W photometry (snr_f140w)
1625-1641 F17.14 --- SNRF150W Signal-to-noise ratio based on the
F150W photometry (snr_f150w)
1643-1662 F20.16 --- SNRF160W ? Signal-to-noise ratio based on
the F160W photometry (snr_f160w)
1664-1682 F19.16 --- SNRF1800W ? Signal-to-noise ratio based on
the F1800W photometry
(snr_f1800w)
1684-1702 F19.15 --- SNRF182M ? Signal-to-noise ratio based on
the F182M photometry (snr_f182m)
1704-1721 F18.14 --- SNRF200W ? Signal-to-noise ratio based on
the F200W photometry (snr_f200w)
1723-1741 F19.15 --- SNRF210M ? Signal-to-noise ratio based on
the F210M photometry (snr_f210m)
1743-1761 F19.14 --- SNRF277W ? Signal-to-noise ratio based on
the F277W photometry (snr_f277w)
1763-1780 F18.14 --- SNRF335M ? Signal-to-noise ratio based on
the F335M photometry (snr_f335m)
1782-1799 F18.14 --- SNRF356W ? Signal-to-noise ratio based on
the F356W photometry (snr_f356w)
1801-1818 F18.14 --- SNRF410M ? Signal-to-noise ratio based on
the F410M photometry (snr_f410m)
1820-1837 F18.14 --- SNRF430M ? Signal-to-noise ratio based on
the F430M photometry (snr_f430m)
1839-1857 F19.16 --- SNRF435W ? Signal-to-noise ratio based on
the F435W photometry (snr_f435w)
1859-1876 F18.14 --- SNRF444W Signal-to-noise ratio based on
the F444w photometry (snr_f444w)
1878-1895 F18.14 --- SNRF460M ? Signal-to-noise ratio based on
the F460M photometry (snr_f460m)
1897-1915 F19.16 --- SNRF475W ? Signal-to-noise ratio based on
the F475W photometry (snr_f475w)
1917-1934 F18.14 --- SNRF480M ? Signal-to-noise ratio based on
the F480M photometry (snr_f480m)
1936-1956 E21.15 --- SNRF606W ? Signal-to-noise ratio based on
the F606W photometry (snr_f606w)
1958-1977 F20.16 --- SNRF770W ? Signal-to-noise ratio based on
the F770W photometry (snr_f770w)
1979-1997 F19.16 --- SNRF775W ? Signal-to-noise ratio based on
the F775W photometry (snr_f775w)
1999-2018 F20.16 --- SNRF814W ? Signal-to-noise ratio based on
the F814W photometry (snr_f814w)
2020-2039 F20.16 --- SNRF850LP ? Signal-to-noise ratio based on
the F850LP photometry
(snr_f850lp)
2041-2051 F11.8 --- SNRHSC-g ? Signal-to-noise ratio based on
the HSC-g photometry (snr_hsc-g)
2053-2064 F12.8 --- SNRHSC-i ? Signal-to-noise ratio based on
the HSC-i photometry (snr_hsc-i)
2066-2076 F11.8 --- SNRHSC-r ? Signal-to-noise ratio based on
the HSC-r photometry (snr_hsc-r)
2078-2089 F12.8 --- SNRHSC-y ? Signal-to-noise ratio based on
the HSC-y photometry (snr_hsc-y)
2091-2102 F12.8 --- SNRHSC-z ? Signal-to-noise ratio based on
the HSC-z photometry (snr_hsc-z)
2104-2115 F12.8 --- SNRHST-f814W ? Signal-to-noise ratio based on
the HST-F814W photometry
(snr_hst-f814w)
2117-2127 F11.7 --- SNRUVISTA-H ? Signal-to-noise ratio based on
the UVISTA-H photometry
(snr_uvista-h)
2129-2139 F11.7 --- SNRUVISTA-J ? Signal-to-noise ratio based on
the UVISTA-J photometry
(snr_uvista-j)
2141-2152 F12.8 --- SNRUVISTA-Ks ? Signal-to-noise ratio based on
the UVISTA-Ks photometry
(snr_uvista-ks)
2154-2165 F12.8 --- SNRUVISTA-Y ? Signal-to-noise ratio based on
the UVISTA-Y photometry
(snr_uvista-y)
2167-2184 F18.16 --- chi2-galaxy Normalized chi- square for
the best-fit eazy-py galaxy model
(chired_galaxy)
2186-2204 F19.15 --- chi2-lzg ? Normalized chi- square for
the best-fit eazy-py low-z galaxy
model (chired_lzg)
2206-2222 F17.15 --- chi2-quasar Normalized chi- square for
the best-fit eazy-py quasar model
(chired_quasar)
2224-2241 F18.15 --- chi2-star Normalized chi- square for
the best-fit eazy-py star model
(chired_star)
2243-2251 F9.7 --- zph-galaxy Photometric redshift based on
the best-fit galaxy template
(zphotgalaxy)
2253-2264 F12.9 --- zph-lzg Photometric redshift based on
the best-fit low-z galaxy
template (zphotlzg)
2266-2274 F9.7 --- zph-quasar Photometric redshift based on
the best-fit quasar template
(zphotquasar)
2276-2292 F17.15 --- e_zph-galaxy Error of the galaxy model
photometric redshift
(zphoterrgalaxy)
2294-2311 F18.16 --- e_zph-lzg Error of the low-z galaxy model
photometric redshift
(zphoterrlzg)
2313-2329 F17.15 --- e_zph-quasar Error of the quasar model
photometric redshift
(zphoterrquasar)
2331-2341 F11.8 --- zsp Spectroscopic redshift compiled
from literature, missing data are
marked with -1 (z_spec)
2343-2358 F16.13 [10-7W] logLbol Bolometric luminosity of the AGN
SED component from the best-fit
CIGALE model (log) (logL_bol)
2360-2377 F18.16 [10-7W] e_logLbol Error of the AGN bolometric
luminosity (log) (logLbolerr)
2379-2398 F20.16 Msun MBH Lower limit black hole mass (log)
(M_BH)
2400-2403 F4.2 --- agnfracAGN Fraction of the AGN emission
computed using least- square
method (agn.fracAGN)
2405-2422 F18.16 --- e_agnfracAGN Error of the AGN emission fraction
(agn.fracAGN_err)
2424-2440 F17.15 mag att.VB90 Attenuation level in V filter
(attenuation.V_B90)
2442-2459 F18.16 mag e_att.VB90 Error of the attenuation level
(attenuation.VB90err)
2461-2480 F20.16 [Msun/yr] log(SFR100Myr) Star formation rate averaged over
100 Myrs (log)
(sfh.sfr100Myrs_log)
2482-2499 F18.16 [Msun/yr] e_log(SFR100Myr) Error of the star formation rate
(log) (sfh.sfr100Myrslogerr)
2501-2517 F17.14 [Msun] logstellarMstar Total stellar mass (log)
(stellar.mstarlog)
2519-2536 F18.16 [Msun] e_logstellarMstar Error of the total stellar mass
(log) (stellar.mstarlog_err)
2538-2554 F17.15 --- univ.redshift Photometric redshift based on the
best-fit CIGALE SED model
(universe.redshift)
2556-2573 F18.16 --- e_univ.redshift Error of the photometric redshift
based on the best-fit CIGALE SED
model (universe.redshift_err)
--------------------------------------------------------------------------------
Acknowledgements:
Irham T. Andika, irham.andika(at)tum.de
(End) Patricia Vannier [CDS] 02-Feb-2024