818 research outputs found
Integral Field Spectroscopy of Mrk 273: Mapping 10^3 km/s Gas Flows and an Off-Nucleus Seyfert 2 Nebula
Integral field optical spectroscopy with the INTEGRAL fiber-based systemis
used to map the extended ionized regions and gas flows in Mrk 273, one of the
closest Ultraluminous Infrared galaxies (ULIRGs).
The Hbeta and [OIII]5007 maps show the presence of two distinct regions
separated by 4'' (3.1 kpc) along position angle (PA) 240. The northeastern
region coincides with the optical nucleus of the galaxy and shows the spectral
characteristics of LINERs. The southwestern region is dominated by [OIII]
emission and is classified as a Seyfert 2. Therefore, in the optical, Mrk 273
is an ultraluminous infrared galaxy with a LINER nucleus and an extended
off-nucleus Seyfert 2 nebula.
The kinematics of the [OIII] ionized gas shows (i) the presence of highly
disturbed gas in the regions around the LINER nucleus, (ii) a high-velocity gas
flow with a peak-to-peak amplitude of 2.4 x 10^3 km/s, and (iii) quiescent gas
in the outer regions (at 3 kpc). We hypothesize that the high-velocity flow is
the starburst-driven superwind generated in an optically obscured nuclear
starburst, and that the quiescent gas is directly ionized by a nuclear source,
like the ionization cones typically seen in Seyfert galaxies.Comment: ApJ Letters, in pres
Integral field optical spectroscopy of a representative sample of ULIRGs: II. Two-dimensional kpc-scale extinction structure
We investigate the two-dimensional kpc-scale structure of the extinction in a
representative sample of local ULIRGs using the Halpha/Hbeta line ratio.We use
optical integral field spectroscopy obtained with the INTEGRAL instrument at
the William Herschel Telescope. Complementary optical and near-IR high angular
resolution HST images have also been used. The extinction exhibits a very
complex and patchy structure in ULIRGs on kpc scales, from basically
transparent regions to others deeply embedded in dust (Av~0.0 to Av~8.0 mag).
Nuclear extinction covers a broad range in Av from 0.6 to 6 mag, 69% of the
nuclei having Av>2.0 mag. Extinction in the external regions is substantially
lower than in the nuclei with 64% of the ULIRGs in the sample having median Av
of less than 2 mag for the entire galaxy. While post-coalescence nuclei tend to
cluster around Av values of 2 to 3 mag, pre-coalescence nuclei appear more
homogeneously distributed over the entire 0.4 mag <Av< 7.7 mag range. For the
average extinction (Av~2.0 derived for the ULIRGs of the sample, the ratio of
the de-reddened to observed SFR values is 6. The extinction-corrected,
Halpha-based SFR ranges from 10 to 300 Msun/yr. For only 28% of the cases the
de-reddened SFR is <20 Msun/yr, whereas for the observed SFR this percentage
increases to 72%. The IR-based SFR is always higher than the optical-based one,
with differences ranging from about 2 to up to 30. The nuclear observed SFR has
an average contribution to the total one of 16% for the entire sample. Once
corrected for extinction, the average value becomes 31%. Because of mostly
extinction effects, the optical (I-band) half-light radius in the sample
galaxies is on average a factor 2.3 larger than the corresponding near-IR
(H-band) value.Comment: To appear in A&
IC5063: A merger with a hidden luminous active nucleus
IC5063 is a nearby galaxy classified as an SO and containing a system of dust lanes parallel to its major optical axis (Danziger, Goss and Wellington, 1981; Bergeron, Durret and Boksenberg, 1983). Extended emission line regions with high excitation properties have been detected over distances of up to 19 kpc from the nucleus. This galaxy has been classified as Seyfert 2 on the basis of its emission line spectrum. These characteristics make IC5063 one of the best candidates for a merger remnant and an excellent candidate for a hidden luminous active nucleus. Based on new broad and narrow band images and long-slit spectroscopy obtained at the ESO 3.6 m telescope, the authors present some preliminary results supporting this hypothesis
Spatially resolved kinematics of the central regions of M83: hidden mass signatures and the role of supernovae
The barred grand-design spiral M83 (NGC 5236) is one of the most studied
galaxies given its proximity, orientation, and particular complexity.
Nonetheless, many aspects of the central regions remain controversial conveying
our limited understanding of the inner gas and stellar kinematics, and
ultimately of the nucleus evolution.
In this work, we present AO VLT-SINFONI data of its central ~235x140 pc with
an unprecedented spatial resolution of ~0.2 arcsec, corresponding to ~4 pc. We
have focused our study on the distribution and kinematics of the stars and the
ionised and molecular gas by studying in detail the Pa_alpha and Br_gamma
emission, the H_2 1-0S(1) line at 2.122 micron and the [FeII] line at 1.644
micron, together with the CO absorption bands at 2.293 micron and 2.323 micron.
Our results reveal a complex situation where the gas and stellar kinematics are
totally unrelated. Supernova explosions play an important role in shaping the
gas kinematics, dominated by shocks and inflows at scales of tens of parsecs
that make them unsuitable to derive general dynamical properties.
We propose that the location of the nucleus of M83 is unlikely to be related
to the off-centre 'optical nucleus'. The study of the stellar kinematics
reveals that the optical nucleus is a gravitationally bound massive star
cluster with M_dyn = (1.1 \pm 0.4)x10^7 M_sun, formed by a past starburst. The
kinematic and photometric analysis of the cluster yield that the stellar
content of the cluster is well described by an intermediate age population of
log T(yr) = 8.0\pm0.4, with a mass of M \simeq (7.8\pm2.4)x10^6 M_sun.Comment: 14 pages, 10 figures, accepted for publication in Ap
Radio monitoring of NGC 7469: Late time radio evolution of SN 2000ft and the circumnuclear starburst in NGC 7469
We present the results of an eight-year long monitoring of the radio emission
from the Luminous Infrared Galaxy (LIRG) NGC 7469, using 8.4 GHz Very Large
Array (VLA) observations at 0.3'' resolution. Our monitoring shows that the
late time evolution of the radio supernova SN 2000ft follows a decline very
similar to that displayed at earlier times of its optically thin phase. The
late time radio emission of SN 2000ft is therefore still being powered by its
interaction with the presupernova stellar wind, and not with the interstellar
medium (ISM). Indeed, the ram pressure of the presupernova wind is \rho_w v_w^2
\approx 7.6E-9 dyn/cm^2, at a supernova age of approximately 2127 days, which
is significantly larger than the expected pressure of the ISM around SN 2000ft.
At this age, the SN shock has reached a distance r_{sh \approx 0.06 pc, and our
observations are probing the interaction of the SN with dense material that was
ejected by the presupernova star about 5820 years prior to its explosion. From
our VLA monitoring, we estimate that the swept-up mass by the supernova shock
after about six years of expansion is \approx 0.29 M_sun, assuming an average
expansion speed of the supernova of 10000 km/s.
We also searched for recently exploded core-collapse supernovae in our VLA
images. Apart from SN 2000ft (S_\nu \approx 1760 microJy at its peak,
corresponding to 1.1E28 erg/s/Hz, we found no evidence for any other radio
supernova (RSN) more luminous than \approx 6.0E26 erg/s/Hz, which suggests that
no other Type IIn SN has exploded since 2000 in the circumnuclear starburst of
NGC 7469.Comment: 10 pages, 5 figures, accepted for publication in MNRA
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