13 research outputs found
Fotometria e calibrazione infrarossi. User Manual
Manuale dove si descrivono le procedure di calibrazione e fotometria infraross
Software di riduzione dati della Camera Infrarossa CAINDR. User Manual
User Manual- Software per la riduzioni dei dati infrarossi della camera CAINDR, situata nel Telescopio Carlos Sanchez (TCS) all'Osservatorio del Teide (Tenerife, Spagna
Uncovering the host galaxy of the -ray-emitting narrow-line Seyfert 1 galaxy FBQS J1644+2619
The discovery of -ray emission from radio-loud narrow-line Seyfert 1
(NLSy1) galaxies has questioned the need for large black hole masses (> 10
M) to launch relativistic jets. We present near-infrared data of the
-ray-emitting NLSy1 FBQS J1644+2619 that were collected using the
camera CIRCE (Canarias InfraRed Camera Experiment) at the 10.4-m Gran
Telescopio Canarias to investigate the structural properties of its host galaxy
and to infer the black hole mass. The 2D surface brightness profile is modelled
by the combination of a nuclear and a bulge component with a S\'ersic profile
with index = 3.7, indicative of an elliptical galaxy. The structural
parameters of the host are consistent with the correlations of effective radius
and surface brightness against absolute magnitude measured for elliptical
galaxies. From the bulge luminosity, we estimated a black hole mass of
(2.10.2) 10 M, consistent with the values
characterizing radio-loud active galactic nuclei.Comment: 5 pages, 3 figures, 1 table. Monthly Notices of the Royal
Astronomical Society Letter, Vol. 469, L11-L1
A near-infrared study of the multi-phase outflow in the type-2 quasar J1509+0434
Based on new near-infrared spectroscopic data from the instrument EMIR on the 10.4 m Gran Telescopio Canarias (GTC) we report the presence of an ionized and warm molecular outflow in the luminous type-2 quasar J150904.22+043441.8 (z = 0.1118). The ionized outflow is faster than its molecular counterpart, although the outflow sizes that we derive for them are consistent within the errors (1.34±0.18 kpc and 1.46±0.20 kpc respectively). We use these radii, the broad emission-line luminosities and in the case of the ionized outflow, the density calculated from the trans-auroral [OII] and [SII] lines, to derive mass outflow rates and kinetic coupling efficiencies. Whilst the ionized and warm molecular outflows represent a small fraction of the AGN power (â€0.033% and 0.0001% of Lbol respectively), the total molecular outflow, whose mass is estimated from an assumed warm-to-cold gas mass ratio of 6Ă 10â5, has a kinetic coupling efficiency of âŒ1.7%Lbol. Despite the large uncertainty, this molecular outflow represents a significant fraction of Lbol and it could potentially have a significant impact on the host galaxy. In addition, the quasar spectrum reveals bright and patchy narrow Paα emission extending out to 4âł (8 kpc) South-East and North-West from the active nucleus.Includes Horizon 202
The host galaxy of the gamma-ray-emitting narrow-line Seyfert 1 galaxy PKS 1502+036
The detection of gamma-ray emission from narrow-line Seyfert 1 galaxies
(NLSy1) has challenged the idea that large black hole (BH) masses (10
M) are needed to launch relativistic jets. We present near-infrared
imaging data of the gamma-ray-emitting NLSy1 PKS 1502+036 obtained with the
Very Large Telescope. Its surface brightness profile, extending to 20
kpc, is well described by the combination of a nuclear component and a bulge
with a Sersic index = 3.5, which is indicative of an elliptical galaxy. A
circumnuclear structure observed near PKS 1502+036 may be the result of galaxy
interactions. A BH mass of about M has been
estimated by the bulge luminosity. The presence of an additional faint disc
component cannot be ruled out with the present data, but this would reduce the
BH mass estimate by only 30%. These results, together with analogous
findings obtained for FBQS J1644+2619, indicate that the relativistic jets in
gamma-ray-emitting NLSy1 are likely produced by massive black holes at the
center of elliptical galaxies.Comment: 5 pages, 2 figures, 1 table, and 2 supplementary figures. Monthly
Notices of the Royal Astronomical Society Letters, Volume 478, Issue 1,
L66-L7
A Reemerging Bright Soft X-Ray State of the Changing-look Active Galactic Nucleus 1ES 1927+654:A Multiwavelength View
1ES1927+654 is a nearby active galactic nucleus (AGN) that has shown an enigmatic outburst in optical/UV followed by X-rays, exhibiting strange variability patterns at timescales of months to years. Here we report the unusual X-ray, UV, and radio variability of the source in its postflare state (2022 Januaryâ2023 May). First, we detect an increase in the soft X-ray (0.3â2 keV) flux from 2022 May to 2023 May by almost a factor of 5, which we call the bright soft state. The hard X-ray 2â10 keV flux increased by a factor of 2, while the UV flux density did not show any significant changes (â€30%) in the same period. The integrated energy pumped into the soft and hard X-rays during this period of 11 months is âŒ3.57 Ă 10 ^50 erg and 5.9 Ă 10 ^49 erg, respectively. From the energetics, it is evident that whatever is producing the soft excess (SE) is pumping out more energy than either the UV or hard X-ray source. Since the energy source presumably is ultimately the accretion of matter onto the supermassive black hole, the SE-emitting region must be receiving the majority of this energy. In addition, the source does not follow the typical diskâcorona relation found in AGNs, neither in the initial flare (from 2017 to 2019) nor in the current bright soft state (2022â2023). We found that the core (<1 pc) radio emission at 5 GHz gradually increased until 2022 March, but showed a dip in 2022 August. The GĂŒdelâBenz relation ( L _radio / L _X-ray ⌠10 ^â5 ), however, is still within the expected range for radio-quiet AGNs, and further follow-up radio observations are currently being undertaken
H alpha Star Formation Rates in Massive Galaxies at z ~ 1
We present a near-infrared spectroscopic study of a stellar mass selected
sample of galaxies at z~1 utilising the LIRIS multi-object spectrograph on the
WHT. We detect continuum, and the H alpha line for our sample, which is one of
the better direct tracers of star formation in external galaxies. We
spectroscopically measure the H alpha emission from 41 massive (M_{*}>10^{10.5}
Msol) galaxies taken from the POWIR Survey with spectroscopic redshifts
0.4<z_{spec}<1.4. We correct our H alpha fluxes for dust extinction by using
multi-wavelength data, and investigate SFR trends with mass and colour. We find
a drop in the fraction of massive galaxies with M_{*}>10^{11} Msol which are
detected in H alpha emission at z<0.9. We furthermore find that the fraction of
galaxies with H alpha emission drops steadily and significantly with redder
(U-B) colours at z~1, and that the SSFR drops with increasing (U-B) colour for
galaxies at all masses. By investigating the SFR-mass relation we find that the
SFR is roughly constant with mass, in possible contrast to previous work, and
that the specific star formation rate (SSFR) is lower in the most massive
galaxies. The scatter in the SFR vs. mass relationship is very small for those
systems with ongoing star formation which suggests that star formation in the
most massive galaxies at z~1 shuts off rather abruptly over <1 Gyr, without an
obvious gradual decline. We furthermore investigate the SFR as a function of
(U-B) colour divided into different mass bins, revealing a tracer of the epoch
of transition from star forming to passive, as a form of star formation
"downsizing". This suggests that the shut off of star formation occurs before
the change in a galaxy's colour. We find that galaxy stellar mass is the
primary driving mechanisms behind the star formation history for these galaxies
and discuss several possible mechanisms for regulating this process.Comment: 20 pages, accepted for publication in MNRA
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A near-infrared study of the multi-phase outflow in the type-2 quasar J1509+0434
Based on new near-infrared spectroscopic data from the instrument EMIR on the 10.4 m Gran Telescopio Canarias (GTC) we report the presence of an ionized and warm molecular outflow in the luminous type-2 quasar J150904.22+043441.8 (z = 0.1118). The ionized outflow is faster than its molecular counterpart, although the outflow sizes that we derive for them are consistent within the errors (1.34±0.18 kpc and 1.46±0.20 kpc respectively). We use these radii, the broad emission-line luminosities and in the case of the ionized outflow, the density calculated from the trans-auroral [OII] and [SII] lines, to derive mass outflow rates and kinetic coupling efficiencies. Whilst the ionized and warm molecular outflows represent a small fraction of the AGN power (â€0.033% and 0.0001% of Lbol respectively), the total molecular outflow, whose mass is estimated from an assumed warm-to-cold gas mass ratio of 6Ă 10â5, has a kinetic coupling efficiency of âŒ1.7%Lbol. Despite the large uncertainty, this molecular outflow represents a significant fraction of Lbol and it could potentially have a significant impact on the host galaxy. In addition, the quasar spectrum reveals bright and patchy narrow Paα emission extending out to 4âł (8 kpc) South-East and North-West from the active nucleus.Includes Horizon 202
Investigating the Puzzling Synchrotron Behaviour of Mrk 421
We investigate the multiwavelength behaviour of the high-energy peaked BL Lac object (HBL) Mrk 421 at redshift z = 0.031 in the period 2007-2015. We use optical photometric, spectroscopic, and polarimetric data and near-infrared data obtained by 35 observatories participating in the GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT), as well as by the Steward Observatory Support of the Fermi Mission. We also employ high-energy data from the Swift (UV and X-rays) satellite to study correlations among emission in different bands.open access journalThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]