10 research outputs found
Another X-ray UFO without a momentum-boosted molecular outflow: ALMA CO(1â0) observations of the galaxy pair IRAS 05054+1718
We present Atacama Large Millimetre/submillimetre Array (ALMA) CO(1â0) observations of the nearby infrared luminous (LIRG) galaxy pair IRAS 05054+1718 (also known as CGCG 468-002), as well as a new analysis of X-ray data of this source collected between 2012 and 2021 using the Nuclear Spectroscopic Telescope Array (NuSTAR), Swift, and the XMM-Newton satellites. The western component of the pair, NED01, hosts a Seyfert 1.9 nucleus that is responsible for launching a powerful X-ray ultra-fast outflow (UFO). Our X-ray spectral analysis suggests that the UFO could be variable or multi-component in velocity, ranging from v/c ⌠â0.12 (as seen in Swift) to v/c ⌠â0.23 (as seen in NuSTAR), and constrains its momentum flux to be poutXâray ⌠(4 ± 2) Ă 1034 g cm sâ2. The ALMA CO(1â0) observations, obtained with an angular resolution of 2.200, although targeting mainly NED01, also include the eastern component of the pair, NED02, a less-studied LIRG with no clear evidence of an active galactic nucleus (AGN). We study the CO(1â0) kinematics in the two galaxies using the 3D-BAROLO code. In both sources we can model the bulk of the CO(1â0) emission with rotating disks and, after subtracting the best-fit models, we detect compact residual emission at S/N = 15 within âŒ3 kpc of the centre. A molecular outflow in NED01, if present, cannot be brighter than such residuals, implying an upper limit on its outflow rate of M outmol . 19 ± 14 M yrâ1 and on its momentum rate of pmolout . (2.7 ± 2.4) Ă 1034 g cm sâ1. Combined with the revised energetics of the X-ray wind, we derive an upper limit on the momentum rate ratio of pmolout / pXoutâray < 0.67. We discuss these results in the context of the expectations of AGN feedback models, and we propose that the X-ray disk wind in NED01 has not significantly impacted the molecular gas reservoir (yet), and we can constrain its effect to be much smaller than expectations of AGN âenergy-drivenâ feedback models. We also consider and discuss the hypothesis of asymmetries of the molecular disk not properly captured by the 3D-BAROLO code. Our results highlight the challenges in testing the predictions of popular AGN disk-wind feedback theories, even in the presence of good-quality multi-wavelength observations
Another X-ray UFO without a momentum-boosted molecular outflow
We present ALMA CO(1-0) observations of the nearby LIRG galaxy pair
IRAS05054+1718 with a new analysis of X-ray data collected between 2012 and
2021 using NuSTAR, Swift, and XMM-Newton. The western component of the pair,
NED01, hosts a Seyfert 1.9 nucleus launching a powerful X-ray UFO. Our X-ray
spectral analysis suggests the UFO could be variable or multi-component in
velocity and constrains its momentum flux to gcms. ALMA CO(1-0) observations include also the
eastern component of the pair, a LIRG with no clear evidence for an AGN. We
study the CO(1-0) kinematics in the two galaxies using the 3D-BAROLO code. In
both sources, we can model the bulk of the CO(1-0) emission with rotating disks
and, after subtracting the best-fit models, we detect compact residual emission
at S/N=15 within kpc from the centre. A molecular outflow in NED01, if
present, cannot be brighter than such residuals, implying an upper limit on its
outflow rate of and on
its momentum rate of gcms. Combined with the revised energetics of the X-ray wind, we
derive an upper limit on the momentum rate ratio of
. We discuss these results in
the context of the expectations of AGN feedback models, and we propose the
X-ray disk wind in NED01 has not significantly impacted the molecular gas
reservoir (yet), and we can constrain its effect to be much smaller than
expectations of AGN ''energy-driven'' feedback models. We also consider and
discuss the hypothesis of asymmetries of the molecular disk not properly
captured by the 3D-BAROLO code. Our results highlight the challenges in testing
the predictions of popular AGN disk-wind feedback theories, even with good
quality multi-wavelength observations.Comment: Accepted by A&
Prestazione motoria e percezione di sĂš. Sviluppo motorio, autoefficacia e pratica sportiva in etĂ evolutiva.
NellâetĂ evolutiva esperienze motorie e sportive positive
contribuiscono allo sviluppo dellâautopercezione
delle competenze motorie. Lo studio si propone di analizzare
e confrontare i livelli di sviluppo motorio e di self-efficacy
motoria in riferimento alle variabili di pratica sportiva
e di genere. Il campione Ăš costituito da quattrocento bambini
(etĂ 8-10 anni) suddiviso secondo il genere e la pratica
sportiva extrascolastica. Nel presente lavoro la pratica
sportiva extrascolastica non determina differenze
significative sullo sviluppo motorio, ma emergono differenze
sullo sviluppo psico-affettivo: i bambini praticanti
avviamento allo sport hanno convinzioni di auto-efficacia
superiori rispetto ai bambini non praticanti attivitĂ sportiva
extrascolastica. I risultati evidenziano differenze
statisticamente significative (p<0,05) nel confronto
di genere, indipendentemente dalla pratica sportiva
extrascolastica, riguardo ai livelli di sviluppo motorio
condizionale e coordinativo. In tutti i test motori non si
riscontrano differenze significative tra bambini praticanti
e non praticanti. Si rilevano differenze statisticamente
significative nella scala di self-efficacy (p<0,01) riguardo
la pratica; differenze significative, inoltre, si rilevano
nel confronto di genere, le femmine evidenziano
un sentimento di auto-efficacia inferiore rispetto ai maschi
Testing the blast-wave AGN feedback scenario in MCG-03-58-007
We report the first Atacama large millimeter/submillimeter array observations of MCG-03- 58-007, a local (z = 0.03236 \ub1 0.00002, this work) AGN (LAGN 3c 1045 erg s-1), hosting a powerful X-ray ultrafast (v = 0.1c) outflow (UFO). The CO(1-0) line emission is observed across 3c18 kpc scales with a resolution of 3c 1 kpc. About 78 per cent of theCO(1-0) luminosity traces a galaxy-size rotating disc. However, after subtracting the emission due to such rotating disc, we detect with a S/N = 20 a residual emission in the central 3c4 kpc. Such residuals may trace a low velocity (vLOS = 170 km s-1) outflow. We compare the momentum rate (P ) and kinetic power (E) of such putative molecular outflow with that of the X-ray UFO and find P mol/P UFO 3c 0.4 and Emol/ EUFO 3c 4
7 10-3. This result is at odds with the energyconserving scenario suggested by the large momentum boosts measured in some other molecular outflows. An alternative interpretation of the residual CO emission would be a compact rotating structure, distinct from the main disc, which would be a factor of 3c10- 100 more extended and massive than typical circumnuclear discs revealed in Seyferts. In conclusion, in both scenarios, our results rule out the hypothesis of a momentum-boosted molecular outflow in this AGN, despite the presence of a powerful X-ray UFO
Dramatic Changes in the Observed Velocity of the Accretion Disk Wind in MCG-03-58-007 Are Revealed by XMM-Newton and NuSTAR
Past X-ray observations of the nearby Seyfert 2 MCG-03-58-007 revealed the presence of a powerful and highly variable disk wind, where two possible phases outflowing with vout1/c ⌠â0.07 and vout2/c ⌠â0.2 were observed. Multi-epoch X-ray observations, covering the period from 2010 to 2018, showed that the lower-velocity component is persistent, as it was detected in all the observations, while the faster phase outflowing with vout2/c ⌠â0.2 appeared to be more sporadic. Here we present the analysis of a new monitoring campaign of MCG-03-58-007 performed in 2019 MayâJune and consisting of four simultaneous XMM-Newton and NuSTAR observations. We confirm that the disk wind in MCG-03-58-007 is persistent, as it is detected in all the observations, and powerful, having a kinetic power that ranges between 0.5% and 10% of the Eddington luminosity. The highly ionized wind (log(Ο/erg cm sâ1) ⌠5) is variable in both the opacity and, remarkably in its velocity. This is the first time where we have observed a substantial variability of the outflowing velocity in a disk wind, which dropped from vout/c ⌠â0.2 (as measured in the first three observations) to vout/c ⌠â0.074 in just 16 days. We conclude that such a dramatic and fast variability of the outflowing velocity could be due to the acceleration of the wind, as recently proposed by Mizumoto et al. Here, the faster wind, seen in the first three observations, is already accelerated to vout/c ⌠â0.2, while in the last observation our line of sight intercepts only the slower, pre-accelerated streamline
Molecular gas kinematics in the nuclear region of nearby Seyfert galaxies with ALMA
Context. The study of the distribution, morphology, and kinematics of cold molecular gas in the nuclear and circumnuclear regions of active galactic nuclei (AGNs) helps to characterise and hence to quantify the impact of the AGNs on the host galaxy over its lifetime.
Aims. We present the analysis of the molecular gas in the nuclear regions of three Seyfert galaxies, NGC 4968, NGC 4845, and MCG-06-30-15, using Atacama Large sub-Millimetre Array (ALMA) observations of the CO(2â1) emission line. The aim is to determine the kinematics of the gas in the central (âŒ1 kpc) region and thereby to probe nuclear fueling and feedback of AGNs.
Methods. We used two different softwares, namely the 3D-Based Analysis of Rotating Object via Line Observations and DiskFit, to model the kinematics of the gas in the molecular disc, and thereby to determine the gas rotation and any kinematical perturbations.
Results. Circular motions dominate the kinematics of the molecular gas in the central discs, mainly in NGC 4845 and MCG-06-30-15; however there is clear evidence of non-circular motions in the central (âŒ1 kpc) region of NGC 4845 and NGC 4968. The strongest non-circular motion is detected in the inner disc of NGC 4968, mainly along the minor kinematic axis, with a velocity âŒ115 km sâ1. Of all DiskFit models, the bisymmetric model is found to give the best fit for NGC 4968 and NGC 4845, indicating that the observed non-circular motions in the inner disc of these galaxies could result from the nuclear barred structure, where the gas streams in elliptical orbits aligned along the bar. If the dynamics of NGC 4968 is modelled as a corotation pattern just outside of the bar, the bar pattern speed becomes Ωb = 52 km sâ1 kpcâ1; the corotation is set at 3.5 kpc; and the inner Lindblad resonance (ILR) ring is Râ=â300 pc, corresponding to the CO emission ring. In the NGC 4968 galaxy, the torques exerted on the gas by the bar are positive in the centre, within the gas nuclear ring, and negative outside. This shows that the gas is transiently trapped in the ILR. The comparison of the CO intensity maps with the map of the cold dust emission shows an absence of CO in the centre of NGC 4968; also the dust distribution and CO emission in and around the centre of NGC 4845 have similar extensions. The 1.2 mm ALMA continuum is peaked and compact in NGC 4968 and MCG-06-30-15, but their CO(2â1) emissions have extended distributions. Allowing the CO-to-H2 conversion factor αCO between 0.8 and 3.2, which is typical of nearby galaxies of the same type, the molecular mass M(H2) is estimated to be âŒ3â
ââ
12â
Ăâ
107âMâ (NGC 4968), âŒ9â
ââ
36â
Ăâ
107âMâ (NGC 4845), and âŒ1â
ââ
4â
Ăâ
107âMâ (MCG-06-30-15).
Conclusions. We conclude that the observed non-circular motions in the molecular disc of NGC 4968 and likely those seen in NGC 4845 are due to the presence of the bar in the nuclear region. We discuss the possibility that the observed pattern in the kinematics might be a consequence of the presence of AGNs, and this might be the case for NGC 4845. At the current spectral and spatial resolution and sensitivity, we cannot claim any strong evidence in these sources of the long sought feedback or feeding effect resulting from the presence of AGNs
Molecular gas kinematics in the nuclear region of nearby Seyfert galaxies with ALMA
Context. The study of the distribution, morphology, and kinematics of
cold molecular gas in the nuclear and circumnuclear regions of active
galactic nuclei (AGNs) helps to characterise and hence to quantify the
impact of the AGNs on the host galaxy over its lifetime. Aims. We
present the analysis of the molecular gas in the nuclear regions of
three Seyfert galaxies, NGC 4968, NGC 4845, and MCG-06-30-15, using
Atacama Large sub-Millimetre Array (ALMA) observations of the CO(2-1)
emission line. The aim is to determine the kinematics of the gas in the
central (similar to 1 kpc) region and thereby to probe nuclear fueling
and feedback of AGNs.
Methods. We used two different softwares, namely the 3D-Based Analysis
of Rotating Object via Line Observations and DiskFit, to model the
kinematics of the gas in the molecular disc, and thereby to determine
the gas rotation and any kinematical perturbations.
Results. Circular motions dominate the kinematics of the molecular gas
in the central discs, mainly in NGC 4845 and MCG-06-30-15; however there
is clear evidence of non-circular motions in the central (similar to 1
kpc) region of NGC 4845 and NGC 4968. The strongest non-circular motion
is detected in the inner disc of NGC 4968, mainly along the minor
kinematic axis, with a velocity similar to 115 km s(-1). Of all DiskFit
models, the bisymmetric model is found to give the best fit for NGC 4968
and NGC 4845, indicating that the observed non-circular motions in the
inner disc of these galaxies could result from the nuclear barred
structure, where the gas streams in elliptical orbits aligned along the
bar. If the dynamics of NGC 4968 is modelled as a corotation pattern
just outside of the bar, the bar pattern speed becomes Omega(b) = 52 km
s(-1) kpc(-1); the corotation is set at 3.5 kpc; and the inner Lindblad
resonance (ILR) ring is R=300 pc, corresponding to the CO emission ring.
In the NGC 4968 galaxy, the torques exerted on the gas by the bar are
positive in the centre, within the gas nuclear ring, and negative
outside. This shows that the gas is transiently trapped in the ILR. The
comparison of the CO intensity maps with the map of the cold dust
emission shows an absence of CO in the centre of NGC 4968; also the dust
distribution and CO emission in and around the centre of NGC 4845 have
similar extensions. The 1.2 mm ALMA continuum is peaked and compact in
NGC 4968 and MCG-06-30-15, but their CO(2-1) emissions have extended
distributions. Allowing the CO-to-H-2 conversion factor alpha(CO)
between 0.8 and 3.2, which is typical of nearby galaxies of the same
type, the molecular mass M(H-2) is estimated to be similar to 3 - 12 x
10(7)M(circle dot) (NGC 4968), similar to 9 - 36 x 10(7) M-circle dot
(NGC 4845), and similar to 1 - 4 x 10(7) M-circle dot (MCG-06-30-15).
Conclusions. We conclude that the observed non-circular motions in the
molecular disc of NGC 4968 and likely those seen in NGC 4845 are due to
the presence of the bar in the nuclear region. We discuss the
possibility that the observed pattern in the kinematics might be a
consequence of the presence of AGNs, and this might be the case for NGC
4845. At the current spectral and spatial resolution and sensitivity, we
cannot claim any strong evidence in these sources of the long sought
feedback or feeding effect resulting from the presence of AGNs
The Source of Leaking Ionizing Photons from Haro11: Clues from HST/COS Spectroscopy of Knots A, B, and C
International audienceUnderstanding the escape of ionizing (Lyman continuum) photons from galaxies is vital for determining how galaxies contributed to reionization in the early universe. While directly detecting the Lyman continuum from high-redshift galaxies is impossible due to the intergalactic medium, low-redshift galaxies in principle offer this possibility but require observations from space. The first local galaxy for which Lyman continuum escape was found is Haro 11, a luminous blue compact galaxy at z = 0.02, where observations with the FUSE satellite revealed an escape fraction of 3.3%. However, the FUSE aperture covers the entire galaxy, and it is not clear from where the Lyman continuum is leaking out. Here we utilize Hubble Space Telescope/Cosmic Origins Spectrograph spectroscopy in the wavelength range 1100-1700 Ă
of the three knots (A, B, and C) of Haro 11 to study the presence of Lyα emission and the properties of intervening gas. We find that all knots have bright Lyα emission. UV absorption lines, originating in the neutral interstellar medium, as well as lines probing the ionized medium, are seen extending to blueshifted velocities of 500 km s-1 in all three knots, demonstrating the presence of an outflowing multiphase medium. We find that knots A and B have large covering fractions of neutral gas, making LyC escape along these sightlines improbable, while knot C has a much lower covering fraction (âČ50%). Knot C also has the the highest Lyα escape fraction, and we conclude that it is the most likely source of the escaping Lyman continuum detected in Haro 11. * Based of observations with the NASA/ESA Hubble Space Telescope