Subscribe to the gold package and get unlimited access to Shamra Academy
Register a new userA panchromatic spatially resolved study of the inner 500pc of NGC1052 -- II: Gas excitation and kinematics
94
0
0.0
(
0
)
Added by
Luis Gabriel Dahmer Hahn
Publication date
2019
fields
Physics
and research's language is
English
Ask ChatGPT about the research
No Arabic abstract
We map the optical and near-infrared (NIR) emission-line flux distributions and kinematics of the inner 320$times$535pc$^2$ of the elliptical galaxy NGC1052. The integral field spectra were obtained with the Gemini Telescope using the GMOS-IFU and NIFS instruments, with angular resolutions of 088 and 01 in the optical and NIR, respectively. We detect five kinematic components: (1 and 2) Two spatially unresolved components, being a broad line region visible in H$alpha$, with a FWHM of $sim$3200km s$^{-1}$ and an intermediate-broad component seen in the [OIII]$lambda lambda$4959,5007 doublet; (3) an extended intermediate-width component with 280<FWHM<450km s$^{-1}$ and centroid velocities up to 400km s$^{-1}$, which dominates the flux in our data, attributed either to a bipolar outflow related to the jets, rotation in an eccentric disc or a combination of a disc and large-scale gas bubbles; (4 and 5) two narrow (FWHM<150km s$^{-1}$) components, one visible in [OIII], and one visible in the other emission lines, extending beyond the field-of-view of our data, which is attributed to large-scale shocks. Our results suggest that the ionization within the observed field of view cannot be explained by a single mechanism, with photoionization being the dominant mechanism in the nucleus with a combination of shocks and photoionization responsible for the extended ionization.
rate research
Read More
We map optical and near-infrared (NIR) stellar population properties of the inner 320$times$535pc$^2$ of the elliptical galaxy NGC1052. The optical and NIR spectra were obtained using the Gemini Integral Field Units of the GMOS instrument and NIFS, respectively. By performing stellar population synthesis in the optical alone, we find that this region of the galaxy is dominated by old (t$>$10Gyr) stellar populations. Using the NIR, we find the nucleus to be dominated by old stellar populations, and a circumnuclear ring with younger ($sim$2.5Gyr) stars. We also combined the optical and NIR datacubes and performed a panchromatic spatially resolved stellar population synthesis, which resulted in a dominance of older stellar populations, in agreement with optical results. We argue that the technique of combining optical and NIR data might be useful to isolate the contribution of stellar population ages with strong NIR absorption bands. We also derive the stellar kinematics and find that the stellar motions are dominated by a high ($sim$240km$cdot$s$^{-1}$) velocity dispersion in the nucleus, with stars also rotating around the center. Lastly, we measure the absorption bands, both in the optical and in the NIR, and find a nuclear drop in their equivalent widths. The favored explanation for this drop is a featureless continuum emission from the low luminosity active galactic nucleus.
We present the spatially resolved gas and stellar kinematics of a sample of ten hidden type 1 AGNs in order to investigate the true nature of the central source and the scaling relation with host galaxy stellar velocity dispersion. The sample is selected from a large number of hidden type 1 AGN, which are identified based on the presence of a broad component in the ha line profile (i.e., full-width-at-half-maximum $>$ $sim$1000 kms), while they are often mis-classified as type 2 AGN because AGN continuum and broad emission lines are weak or obscured in the optical spectral range. We used the Blue Channel Spectrograph at the 6.5-m MMT (Multiple Mirror Telescope) to obtain long-slit data. We detected a broad hb for only two targets, however, the presence of a strong broad ha indicates that these AGNs are low-luminosity type 1 AGNs. We measured the velocity, velocity dispersion and flux of stellar continuum and gas emission lines (i.e., hb and oiii) as a function of distance from the center with a spatial scale of 0.3 arcsec pixel$^{-1}$. Spatially resolved gas kinematics traced by hb or oiii are generally similar to stellar kinematics except for the very center, where signatures of gas outflows are detected. We compare the luminosity-weighted effective stellar velocity dispersion with black hole mass, finding that these hidden type 1 AGN with relatively low back hole mass follow the scaling relation of the reverberation-mapped type 1 AGN and more massive inactive galaxies. }
We present detailed observations of photoionization conditions and galaxy kinematics in eleven z$=1.39-2.59$ radio-loud quasar host galaxies. Data was taken with OSIRIS integral field spectrograph (IFS) and the adaptive optics system at the W.M. Keck Observatory that targeted nebular emission lines (H$beta$,[OIII],H$alpha$,[NII]) redshifted into the near-infrared (1-2.4 micron). We detect extended ionized emission on scales ranging from 1-30 kpc photoionized by stars, shocks, and active galactic nuclei (AGN). Spatially resolved emission-line ratios indicate that our systems reside off the star formation and AGN-mixing sequence on the Baldwin, Phillips $&$ Terlevich (BPT) diagram at low redshift. The dominant cause of the difference between line ratios of low redshift galaxies and our sample is due to lower gas-phase metallicities, which are 2-5$times$ less compared to galaxies with AGN in the nearby Universe. Using gas velocity dispersion as a proxy to stellar velocity dispersion and dynamical mass measurement through inclined disk modeling we find that the quasar host galaxies are under-massive relative to their central supermassive black hole (SMBH) mass, with all systems residing off the local scaling ($M_{bullet}-sigma~$,$M_{bullet}-M_{*}~$) relationship. These quasar host galaxies require substantial growth, up to an order of magnitude in stellar mass, to grow into present-day massive elliptical galaxies. Combining these results with part I of our sample paper (Vayner et al. 2021) we find evidence for winds capable of causing feedback before the AGN host galaxies land on the local scaling relation between black hole and galaxy stellar mass, and before the enrichment of the ISM to a level observed in local galaxies with AGN.
In the second work of this series, we analyse the connection between the availability of gas and the position of a region with respect to the spatially resolved main sequence (MS) relation. Following the procedure presented in Paper I we obtain 500pc scales estimates of stellar mass and star formation rate surface densities ($Sigma_{star}$ and $Sigma_{rm{SFR}}$). Our sample consists of five face-on, grand design spiral galaxies located on the MS. Thanks to HI 21cm and $^{12}$CO(2-1) maps, we connect the gas surface densities and gas fractions to the observed star formation properties of each region. We find that the spatially resolved MS ($sigma=0.23$ dex) is the combination of two relations: the Kennicutt-Schmidt law ($sigma=0.19$ dex) and the molecular gas MS (MGMS, $sigma=0.22$ dex); $Sigma_{star}$, $Sigma_{rm{SFR}}$ and the surface density of the molecular gas, $Sigma_{rm{H_2}}$, define a 3D relation as proposed by citet{2019ApJ...884L..33L}. We find that $Sigma_{rm{H_2}}$ steadily increases along the MS relation, varies little towards higher $Sigma_{rm{SFR}}$ at fixed stellar surface densities (not enough to sustain the change in SFR), and it is almost constant perpendicular to the relation. The surface density of neutral gas ($Sigma_{rm{HI}}$) is constant along the MS, and increases in its upper envelop. $Sigma_{rm{SFR}}$ can be expressed as a function of $Sigma_{star}$ and $Sigma_{rm{HI}}$, following the Equation: $logSigma_{rm{SFR}}$ = 0.97$logSigma_{star}$ + 1.99$logSigma_{rm{HI}}$ - 11.11. Finally, we show that f$_{rm{gas}}$ increases significantly towards the starburst region in the $logSigma_{star}$ - $logSigma_{rm{SFR}}$ plane, accompanied by a slight increase in SFE.
The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) aims at tracing and characterizing ionized gas outflows and their impact on star formation in a statistical sample of X-ray selected Active Galactic Nuclei (AGN) at z$sim$2. We present the first SINFONI results for a sample of 21 Type-1 AGN spanning a wide range in bolometric luminosity (log $mathrm{L_{bol}}$ = 45.4-47.9 erg/s). The main aims of this paper are determining the extension of the ionized gas, characterizing the occurrence of AGN-driven outflows, and linking the properties of such outflows with those of the AGN. We use Adaptive Optics-assisted SINFONI observations to trace ionized gas in the extended narrow line region using the [OIII]5007 line. We classify a target as hosting an outflow if its non-parametric velocity of the [OIII] line, $mathrm{w_{80}}$, is larger than 600 km/s. We study the presence of extended emission using dedicated point-spread function (PSF) observations, after modelling the PSF from the Balmer lines originating from the Broad Line Region. We detect outflows in all the Type-1 AGN sample based on the $mathrm{w_{80}}$ value from the integrated spectrum, which is in the range 650-2700 km/s. There is a clear positive correlation between $mathrm{w_{80}}$ and the AGN bolometric luminosity (99% correlation probability), but a weaker correlation with the black hole mass (80% correlation probability). A comparison of the PSF and the [OIII] radial profile shows that the [OIII] emission is spatially resolved for $sim$35% of the Type-1 sample and the outflows show an extension up to $sim$6 kpc. The relation between maximum velocity and the bolometric luminosity is consistent with model predictions for shocks from an AGN driven outflow. The escape fraction of the outflowing gas increase with the AGN luminosity, although for most galaxies, this fraction is less than 10%.
Log in to be able to interact and post comments
comments
Fetching comments
Sign in to be able to follow your search criteria
