Panoramic Spectroscopy of Sy Galaxies with elongated radio structures

AbstractWe have studied the ionized gas and stellar kinematics in several galaxies with active nuclei and elongated radio structures using 3D spectroscopy. The observations were performed at the SAO RAS 6-m telescope with the integral-field spectrograph MPFS (Afanasiev et al. 2001) and with a scanning Fabry-Perot interferometer (FPI) in the multimode device SCORPIO (Afanasiev & Moiseev 2005). Based on these data the intensity maps and velocity fields in the different emission lines of the ionizing gas were constructed. Using the lines-ratio diagrams we tried to search a source of the gas ionization: an active nucleus, hot young stars or shock waves.

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Gas Motion Mapping for Three Seyfert Galaxies

Open Astronomy ◽

10.1515/astro-2017-0325 ◽

2011 ◽

Vol 20 (3) ◽

Author(s):

A. Smirnova ◽

A. Moiseev ◽

I. Katkov ◽

V. Afanasiev

Keyword(s):

Active Galactic Nuclei ◽

Galactic Nuclei ◽

Seyfert Galaxies ◽

Velocity Fields ◽

Emission Lines ◽

Ionized Gas ◽

Preliminary Results ◽

Fabry Perot ◽

Integral Field Spectrograph ◽

Integral Field

AbstractWe report the preliminary results of a kinematical study of three Seyfert galaxies selected from a sample of nearby active galactic nuclei observed using 3D spectroscopy. The observations were performed at the prime focus of the 6 m telescope of SAO RAS with the integral-field spectrograph MPFS and with a scanning Fabry-Pérot interferometer, installed on the multimode device SCORPIO. Based on these data, the monochromatic maps and velocity fields in different emission lines were constructed. We have detected the nuclear outflow or ionized gas motions associated with a radio jet in all the circumnuclear regions of these galaxies.

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Integral Field Spectroscopy of z ~ 0.1 QSO Host Galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310006642 ◽

2009 ◽

Vol 5 (S267) ◽

pp. 334-334

Author(s):

Dading Nugroho ◽

Knud Jahnke ◽

Bernd Husemann ◽

Katherine Inskip ◽

Sebastian F. Sánchez ◽

...

Keyword(s):

Velocity Fields ◽

Emission Lines ◽

Gas Velocity ◽

Host Galaxies ◽

Limited Sample ◽

Integral Field Spectroscopy ◽

Field Spectroscopy ◽

Integral Field Spectrograph ◽

Integral Field

We observed a volume-limited sample of 19 luminous type 1 QSO host galaxies at MV ~ −23 mag and redshift 0.06 < z < 0.2 (Jahnke et al. 2004) using the VLT/VIMOS Integral Field Spectrograph. After removal of the QSO contribution (using the method of Husemann et al. 2008), we construct 2D intensity maps and gas velocity fields of the host galaxies in the Hα and [O iii] emission lines. Two representative cases are shown in Figure 1.

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Ionized gas kinematics of massive elliptical galaxies in CALIFA and in cosmological zoom-in simulations

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936441 ◽

2020 ◽

Vol 635 ◽

pp. A41

Author(s):

Jan Florian ◽

Bodo Ziegler ◽

Michaela Hirschmann ◽

Polychronis Papaderos ◽

Ena Choi ◽

...

Keyword(s):

Radial Profile ◽

Major Axis ◽

Velocity Fields ◽

Host Galaxies ◽

Ionized Gas ◽

Massive Galaxies ◽

Gas Kinematics ◽

Major Merger ◽

Ordered Motion ◽

Integral Field

Context. Powerful active galactic nuclei (AGN) are supposed to play a key regulatory role on the evolution of their host galaxies by shaping the thermodynamic properties of their gas component. However, little is known as to the nature and the visibility timescale of the kinematical imprints of AGN-driven feedback. Gaining theoretical and observational insights into this subject is indispensable for a thorough understanding of the AGN-galaxy coevolution and could yield empirical diagnostics for the identification of galaxies that have experienced a major AGN episode in the past. Aims. We present an investigation of kinematical imprints of AGN feedback on the warm ionized gas medium (WIM) of massive early-type galaxies (ETGs). To this end, we take a two-fold approach that involves a comparative analysis of Hα velocity fields in 123 local ETGs from the CALIFA (Calar Alto Legacy Integral Field Area Survey) integral field spectroscopy survey with 20 simulated galaxies from high-resolution hydrodynamic cosmological SPHgal simulations. The latter were resimulated for two modeling setups, one with and another without AGN feedback. Methods. In order to quantify the effects of AGN feedback on gas kinematics, we measured three parameters that probe deviations from simple regular rotation by using the kinemetry package. These indicators trace the possible presence of distinct kinematic components in Fourier space (k3, 5/k1), variations in the radial profile of the kinematic major axis (σPA), and offsets between the stellar and gas velocity fields (Δϕ). These quantities were monitored in the simulations from a redshift 3 to 0.2 to assess the connection between black hole accretion history, stellar mass growth, and the kinematical perturbation of the WIM. Results. Observed local massive galaxies show a broad range of irregularities, indicating disturbed warm gas motions, which is irrespective of being classified via diagnostic lines as AGN or not. Simulations of massive galaxies with AGN feedback generally exhibit higher irregularity parameters than without AGN feedback, which is more consistent with observations. Besides AGN feedback, other processes like major merger events or infalling gas clouds can lead to elevated irregularity parameters, but they are typically of shorter duration. More specifically, k3, 5/k1 is most sensitive to AGN feedback, whereas Δϕ is most strongly affected by gas infall. Conclusions. We conclude that even if the general disturbance of the WIM velocity is not a unique indicator for AGN feedback, irregularity parameters that are high enough to be consistent with observations can only be reproduced in simulations with AGN feedback. Specifically, an elevated value for the deviation from simple ordered motion is a strong sign for previous events of AGN activity and feedback.

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The MURALES survey

Astronomy and Astrophysics ◽

10.1051/0004-6361/202039062 ◽

2020 ◽

Vol 645 ◽

pp. A12

Author(s):

B. Balmaverde ◽

A. Capetti ◽

A. Marconi ◽

G. Venturi ◽

M. Chiaberge ◽

...

Keyword(s):

Emission Line ◽

Large Scale ◽

Line Emission ◽

Emission Region ◽

Gas Velocity ◽

Ionized Gas ◽

Large Scale Structures ◽

Scale Structures ◽

Integral Field Spectrograph ◽

Integral Field

We present the final observations of a complete sample of 37 radio galaxies from the Third Cambridge Catalogue (3C) with redshift < 0.3 and declination < 20° obtained with the VLT/MUSE optical integral field spectrograph. These data were obtained as part of the MUse RAdio Loud Emission line Snapshot (MURALES) survey with the main goal of exploring the AGN feedback process in the most powerful radio sources. We present the data analysis and, for each source, the resulting emission line images and the 2D gas velocity field. Thanks to the unprecedented depth these observations reveal emission line regions (ELRs) extending several tens of kiloparsec in most objects. The gas velocity shows ordered rotation in 25 galaxies, but in several sources it is highly complex. We find that the 3C sources show a connection between radio morphology and emission line properties. In the ten FR I sources the line emission region is generally compact, only a few kpc in size; only in one case does it exceed the size of the host. Conversely, all but two of the FR II galaxies show large-scale structures of ionized gas. The median extent is 16 kpc with the maximum reaching a size of ∼80 kpc. There are no apparent differences in extent or strength between the ELR properties of the FR II sources of high and low gas excitation. We confirm that the previous optical identification of 3C 258 is incorrect: this radio source is likely associated with a quasi-stellar object at z ∼ 1.54.

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The distant (z = 0.471) radiogalaxy 3C 435 A with the integral field spectrograph TIGER

International Astronomical Union Colloquium ◽

10.1017/s025292110002306x ◽

1995 ◽

Vol 149 ◽

pp. 250-253

Author(s):

B. Rocca-Volmerange ◽

G. Adam ◽

P. Ferruit ◽

R. Bacon

Keyword(s):

Energy Distribution ◽

Galaxy Evolution ◽

Large Degree ◽

Emission Lines ◽

Image Point ◽

Redshift Galaxy ◽

Stellar Energy ◽

Integral Field Spectrograph ◽

Intermediate Redshift ◽

Integral Field

The distant radiogalaxies recently discovered at the most remote distances (z≥3.5) are among the best cosmological targets. However so various features caracterize these galaxies (red stellar energy distribution, huge emission lines, high density of galaxy companions, alignment of ultraviolet and radio axes, large degree of polarisation) that their structures are not simple to understand. Stellar populations will only become the best indicators of evolution of galaxies if these structures are clearly understood from a two-dimension spectroscopy on each image point. The integral field spectrograph TIGER is a unique instrument at the CFHT to give details on the nature and velocities of the various components of distant radiogalaxies.We present the observations with TIGER of an intermediate-redshift galaxy 3C435A (z=0.471) (Rocca-Volmerange et al, 1994). The two nebular lines [OII], [OIII] and the largely extended stellar continua are observable, allowing to date galaxy with the help of our evolution model. The present and past star formation activities and the origin of alignment will be thus analysed in terms of galaxy evolution.

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Reduction of 3D Spectral Data, Obtained with the 6-meter Telescope

International Astronomical Union Colloquium ◽

10.1017/s0252921100023216 ◽

1995 ◽

Vol 149 ◽

pp. 308-310

Author(s):

V. V. Vlasiouk

Keyword(s):

Spectral Data ◽

Spectral Methods ◽

Data Reduction ◽

Simultaneous Detection ◽

Personal Computers ◽

Specialized Software ◽

Fabry Perot ◽

Extended Sources ◽

Integral Field Spectrograph ◽

Integral Field

Development of 3D spectral methods on the 6-meter telescope prompted the necessity of creating specialized software for data reduction, adapted to personal computers IBM AT/386/486 class. We had to concentrate our efforts on preparing the software for bidimensional spectral data produced by Multi-Pupil Integral Field Spectrograph of the 6-meter telescope (MPFS) and analog of panoramic spectrophotometer with spectral channeling, using scanning Fabry-Perot interferometer (PYTHEAS-6).MPFS - analog of spectrograph TIGER (Courtes et al., 1988), developed for the 6-meter telescope, provides bidimensional spectroscopy of extended sources, allowing the simultaneous detection of 99 individual spectra, produced by a lens raster from 9 by 11 microlenses. The main features of this instrument are described in (Afanasiev et al, 1994).

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Feeding and feedback in the active nucleus of Mrk 1157 probed with the Gemini Near-Infrared Integral-Field Spectrograph

Monthly Notices of the Royal Astronomical Society ◽

10.1111/j.1365-2966.2011.19441.x ◽

2011 ◽

Vol 417 (4) ◽

pp. 2752-2769 ◽

Cited By ~ 58

Author(s):

Rogemar A. Riffel ◽

Thaisa Storchi-Bergmann

Keyword(s):

Near Infrared ◽

Active Nucleus ◽

Integral Field Spectrograph ◽

Integral Field

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An outflow in the Seyfert ESO 362-G18 revealed by Gemini-GMOS/IFU observations

Astronomy and Astrophysics ◽

10.1051/0004-6361/201731671 ◽

2018 ◽

Vol 614 ◽

pp. A94 ◽

Cited By ~ 7

Author(s):

Pedro K. Humire ◽

Neil M. Nagar ◽

Carolina Finlez ◽

Verónica Firpo ◽

Roy Slater ◽

...

Keyword(s):

Galactic Disk ◽

Position Angle ◽

Morphological Type ◽

Emission Lines ◽

Stellar Kinematics ◽

Mean Velocity ◽

Gas Kinematics ◽

Gaussian Fit ◽

Kinematic Position ◽

Integral Field Spectrograph

We present two-dimensional stellar and gaseous kinematics of the inner 0.7 × 1.2 kpc2 of the Seyfert 1.5 galaxy ESO 362-G18, derived from optical (4092–7338 Å) spectra obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of ≈170 pc and spectral resolution of 36 km s−1. ESO 362-G18 is a strongly perturbed galaxy of morphological type Sa or S0/a, with a minor merger approaching along the NE direction. Previous studies have shown that the [O III] emission shows a fan-shaped extension of ≈10′′ to the SE. We detect the [O III] doublet, [N II] and Hα emission lines throughout our field of view. The stellar kinematics is dominated by circular motions in the galaxy plane, with a kinematic position angle of ≈137° and is centred approximately on the continuum peak. The gas kinematics is also dominated by rotation, with kinematic position angles ranging from 122° to 139°, projected velocity amplitudes of the order of 100 km s−1, and a mean velocity dispersion of 100 km s−1. A double-Gaussian fit to the [O III]λ5007 and Hα lines, which have the highest signal to noise ratios of the emission lines, reveal two kinematic components: (1) a component at lower radial velocities which we interpret as gas rotating in the galactic disk; and (2) a component with line of sight velocities 100–250 km s−1 higher than the systemic velocity, interpreted as originating in the outflowing gas within the AGN ionization cone. We estimate a mass outflow rate of 7.4 × 10−2 M⊙ yr−1 in the SE ionization cone (this rate doubles if we assume a biconical configuration), and a mass accretion rate on the supermassive black hole (SMBH) of 2.2 × 10−2 M⊙ yr−1. The total ionized gas mass within ~84 pc of the nucleus is 3.3 × 105 M⊙; infall velocities of ~34 km s−1 in this gas would be required to feed both the outflow and SMBH accretion.

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High Spatial Resolution Integral Field Spectroscopy of extended Ionized Gas around three Quasars

International Astronomical Union Colloquium ◽

10.1017/s0252921100023071 ◽

1995 ◽

Vol 149 ◽

pp. 254-256

Author(s):

F. Durret ◽

E. Pécontal ◽

P. Petitjean ◽

J. Bergeron

Keyword(s):

Spatial Resolution ◽

Spectral Resolution ◽

Rest Frame ◽

High Spatial Resolution ◽

Wavelength Region ◽

Ionized Gas ◽

Integral Field Spectroscopy ◽

Field Spectroscopy ◽

Integral Field Spectrograph ◽

Integral Field

Three quasars, Ton 616, 4C 37.43 and PKS 2251+113 (Stockton and MacKenty 1987) were observed in 1992 at the 3.6 m CFH telescope with the Integral Field Spectrograph TIGER (Courtès et al. 1987, Pécontal 1991) under subarcsecond seeing (0.5 - 0.7”). The spatial sampling was 0.39” in a field 7 by 7 ”, and the spectral resolution 8 ÅFWHM in the Hβ - [OIII]λ 5007 wavelength region (in the rest frame of the objects). The scaling is 4.5, 5.9 and 5.3 kpc.arcsec−1 for Ton 616, 4C 37.43 and PKS 2251+113 respectively (H0 = 75 km.s−1.Mpc−1). The data were reduced with the software developed at Observatoire de Lyon by Rousset, Bacon and Pécontal (Rousset 1992). A detailed account of our results is reported in Durret et al. 1994.

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