scholarly journals Simulating gas kinematic studies of high-redshift galaxies with the HARMONI integral field spectrograph

2020 ◽  
Vol 498 (2) ◽  
pp. 1891-1904
Author(s):  
Mark L A Richardson ◽  
Laurence Routledge ◽  
Niranjan Thatte ◽  
Matthias Tecza ◽  
Ryan C W Houghton ◽  
...  
Keyword(s):  
Near Infrared ◽  
High Redshift ◽  
Line Emission ◽  
High Angular Resolution ◽  
High Redshift Galaxies ◽  
Gas Kinematics ◽  
Post Process ◽  
Kinematic Studies ◽  
Integral Field Spectrograph ◽  
Integral Field

ABSTRACT We present simulated observations of gas kinematics in a galaxy formed in a 10 pc resolution cosmological simulation with the hydrodynamical +   N-body code ramses, using the new ramses2hsim pipeline with the simulated observing pipeline (hsim) for the Extremely Large Telescope High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph (HARMONI IFS). We post-process the galaxy's gas kinematics and Hα line emission for each simulation cell, and integrate the emission to produce an extinction-corrected input cube. We then simulate observations of the input cube with HARMONI, for a range of exposure times, spatial sampling, and spectral resolution. We analyse the mock observations to recover galaxy properties such as its kinematics and compare with the known simulation values. We investigate the cause of biases between the ‘real’ and ‘observed’ kinematic values, demonstrating the sensitivity of the inferred rotation curve to knowledge of the instrument’s point spread function.

scholarly journals Near-IR Integral Field Spectroscopy of the central region of NGC 5929

2014 ◽  
Vol 10 (S309) ◽  
pp. 339-339
Author(s):  
Rogemar A. Riffel ◽  
Thaisa Storchi-Bergmann ◽  
Rogério Riffel
Keyword(s):  
Emission Line ◽  
Near Infrared ◽  
Line Emission ◽  
Linear Structure ◽  
Emission Lines ◽  
Line Profiles ◽  
Gas Kinematics ◽  
Systemic Velocity ◽  
Integral Field Spectrograph ◽  
Integral Field

AbstractWe present two-dimensional (2D) near-infrared spectra of the inner 300×300 pc2 of the Seyfert 2 galaxy NGC 5929 at a spatial resolution of ~20 pc obtained with the Gemini Near infrared Integral Field Spectrograph (NIFS). We present 2D maps for the emission line flux distributions and kinematics and report the discovery of a linear structure ~300 pc in extent and of ~50 pc in width oriented perpendicular to the radio jet, showing broadened emission-line profiles.While over most of the field the emission-line profiles have full-widths-at-half-maximum (FWHM) of ~210 km/s, at a linear structure perpendicular do the radio jet the emission-line FWHMs are twice this value, and are due to two velocity components, one blueshifted and the other redshifted relative to the systemic velocity. We attribute these velocities to an outflow from the nucleus which is launched perpendicular to the radio jet. We reported the detection of this peculiar outflow in Riffel, Storchi-Bergmann & Riffel (2014a), where more details of the analysis can be found. Since, NGC 5929 has a Type 2 nucleus, this detection implies that: (1) both ionizing radiation and relativistic particles are escaping through holes in the torus perpendicular to the radio jet; and/or (2) the torus is also outflowing, as proposed by recent models of tori as winds from the outer parts of an accretion flow; or (3) the torus is absent in NGC 5929.At other locations the gas kinematics is dominated by rotation in a disk, although some evidences of interaction of the radio jet with the emitting gas are seen as a broadening of the line profiles at the locations of the radio structures.The flux distributions for the [P ii], [Fe ii], H i and H2 emission lines show that the line emission is more extended along the PA = 60/240^, extending to up to 1.5” to both sides of the nucleus, while to the perpendicular direction (PA = -30/150^) the emission is extended to 0.7” from the nucleus. The flux distributions of all emission lines show a good correlation with radio the radio structures, with the two peak of emission associated to the soutwestern and northeastern radio knots. Some differences are observed among distinct emission lines. While the [Fe ii] and H2 emission peak at the location of the soutwestern radio structure at 0.6” from the nucleus, the H i recombination lines present the their highest fluxes at the location of the northeastern radio hotspot at 0.5” from the nucleus. Another difference is that the H2 emission is less collimated than that for other lines, being more extended perpendicularly to the radio jet. A detailed analysis of the line emission and kinematics will be presented in Riffel, Storchi-Bergmann & Riffel (2014b).

scholarly journals Simulated stellar kinematics studies of high-redshift galaxies with the HARMONI Integral Field Spectrograph

2016 ◽  
Vol 458 (3) ◽  
pp. 2405-2422 ◽  
Author(s):  
S. Kendrew ◽  
S. Zieleniewski ◽  
R. C. W. Houghton ◽  
N. Thatte ◽  
J. Devriendt ◽  
...  
Keyword(s):  
High Redshift ◽  
Stellar Kinematics ◽  
High Redshift Galaxies ◽  
Integral Field Spectrograph ◽  
Integral Field ◽  
Redshift Galaxies

scholarly journals Near-infrared Integral-Field Spectrograph (NIFS): An Instrument Proposed for Gemini

1999 ◽  
Vol 16 (3) ◽  
pp. 273-287 ◽  
Author(s):  
Peter J. McGregor ◽  
Peter Conroy ◽  
Gabe Bloxham ◽  
Jan van Harmelen
Keyword(s):  
Control System ◽  
Near Infrared ◽  
High Efficiency ◽  
Low Cost ◽  
High Redshift ◽  
Target Velocity ◽  
Wide Range ◽  
Integral Field Spectrograph ◽  
Field Unit ◽  
Integral Field

AbstractIn late 1998 the International Gemini Project Office identified a need for a low cost, near-infrared spectrograph to be commissioned on the Gemini South telescope on the shortest possible timescale. In response, the Research School of Astronomy and Astrophysics of the Australian National University proposed to design, construct, and commission a near-infrared, integral-field spectrograph on Gemini. The science drivers and novel design of the Near-infrared Integral-Field Spectrograph (NIFS) are described in this paper. NIFS will achieve significant economies in cost and schedule in several ways:• By addressing targeted science with high efficiency. NIFS will primarily target velocity measurements in galaxies to study the demographics of black holes in galactic nuclei and the evolution of structural properties in high redshift galaxies. However, NIFS will also be applied to a wide range of general astronomical topics, but these will not dictate the instrument design.• By adopting a largely fixed-format design. A 3·2″ × 3·2″ ‘stair-case’ integral field unit (IFU) will feed a near-infrared spectrograph with four fixed-angle gratings mounted on a single grating wheel. A single, fixed-format camera will form the spectral image on a 2048 × 2048 Rockwell HgCdTe HAWAII-2 array. Two-pixel spectral resolving powers of ∼5400 will be achieved with complete wavelength coverage in each of the J, H, and K photometric bands through 32 optimally sampled 0·1″ wide slitlets. The velocity resolution of ∼55 km s−1 will be sufficient to achieve the targeted science objectives, and will allow software rejection of OH airglow lines.• By packaging the NIFS instrument within a duplicate of the Near-Infrared Imager (NIRI) cryostat. The NIRI cryostat, On-Instrument Wavefront Sensor (OIWFS), detector focusing mechanism, control system, and EPICS software will all be duplicated with only minimal change. Construction of the duplicate NIRI cryostat, OIWFS, and control system will be done by the University of Hawaii.

scholarly journals Evidence for an accreting massive black hole in He 2–10 from adaptive optics integral field spectroscopy

2020 ◽  
Vol 494 (2) ◽  
pp. 2004-2011 ◽  
Author(s):  
Rogemar A Riffel
Keyword(s):  
Black Hole ◽  
Adaptive Optics ◽  
Near Infrared ◽  
Dwarf Galaxy ◽  
Line Emission ◽  
Massive Black Hole ◽  
Star Forming ◽  
Star Forming Regions ◽  
Integral Field Spectrograph ◽  
Integral Field

ABSTRACT Henize 2–10 is a blue dwarf galaxy with intense star formation and one the most intriguing question about it is whether or not it hosts an accreting massive black hole. We use H and K-band integral field spectra of the inner 130 pc × 130 pc of He 2–10 to investigate the emission and kinematics of the gas at unprecedented spatial resolution. The observations were done using the Gemini Near-Infrared Integral Field Spectrograph (NIFS) operating with the ALTAIR adaptive optics module and the resulting spatial resolutions are 6.5 and 8.6 pc in the K and H bands, respectively. Most of the line emission is due to excitation of the gas by photoionization and shocks produced by the star forming regions. In addition, our data provide evidence of emission of gas excited by an active galactic nucleus located at the position of the radio and X-ray sources, as revealed by the analysis of the emission-line ratios. The emission lines from the ionized gas in the field present two kinematic components: one narrow with a velocity field suggesting a disc rotation and a broad component due to winds from the star forming regions. The molecular gas shows only the narrow component. The stellar velocity dispersion map presents an enhancement of about 7 km s−1 at the position of the black hole, consistent with a mass of $1.5^{+1.3}_{-1.3}\times 10^6$ M⊙.

scholarly journals Ionized and hot molecular outflows in the inner 500 pc of NGC 1275

2020 ◽  
Vol 496 (4) ◽  
pp. 4857-4873
Author(s):  
Rogemar A Riffel ◽  
Thaisa Storchi-Bergmann ◽  
Nadia L Zakamska ◽  
Rogério Riffel
Keyword(s):  
Near Infrared ◽  
Line Emission ◽  
Seyfert Galaxy ◽  
Gas Phases ◽  
Gas Kinematics ◽  
The Galaxy ◽  
Stellar Velocity ◽  
Mass Outflow ◽  
Integral Field Spectrograph ◽  
Ngc 1275

ABSTRACT The role of feedback from active galactic nuclei (AGNs) in the evolution of galaxies is still not fully understood, mostly due to the lack of observational constraints in the multiphase gas kinematics on the 10–100 pc scales. We have used the Gemini Near-Infrared Integral Field Spectrograph (NIFS) to map the molecular and ionized gas kinematics in the inner 900 × 900 pc2 of the Seyfert galaxy NGC 1275 at a spatial resolution of ∼70 pc. From the fitting of the CO absorption bandheads in the K band, we derive a stellar velocity dispersion of 265 ± 26 km s−1, which implies a black hole mass of $M_{\rm SMBH}=1.1^{+0.9}_{-0.5}\times 10^9$ M⊙. We find hot (T ≳ 1000 K) molecular and ionized outflows with velocities of up to 2000 km s−1 and mass outflow rates of $2.7\times 10^{-2}$  and $1.6\, {\rm M_\odot }$ yr−1, respectively, in each of these gas phases. The kinetic power of the ionized outflows corresponds to only 0.05 per cent of the luminosity of the AGN of NGC 1275, indicating that they are not powerful enough to provide significant AGN feedback, but may be effective in redistributing the gas in the central region of the galaxy. The AGN-driven outflows seem to be responsible for the shocks necessary to produce the observed H2 and [Fe ii] line emission.

scholarly journals The MURALES survey

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.

scholarly journals Gone with the heat: a fundamental constraint on the imaging of dust and molecular gas in the early Universe

2016 ◽  
Vol 3 (6) ◽  
pp. 160025 ◽  
Author(s):  
Zhi-Yu Zhang ◽  
Padelis P. Papadopoulos ◽  
R. J. Ivison ◽  
Maud Galametz ◽  
M. W. L. Smith ◽  
...  
Keyword(s):  
Structural Characteristics ◽  
High Redshift ◽  
Line Emission ◽  
Velocity Fields ◽  
Molecular Gas ◽  
Gas Velocity ◽  
High Redshift Galaxies ◽  
Mass Distributions ◽  
Line Imaging ◽  
Cold Dust

Images of dust continuum and carbon monoxide (CO) line emission are powerful tools for deducing structural characteristics of galaxies, such as disc sizes, H 2 gas velocity fields and enclosed H 2 and dynamical masses. We report on a fundamental constraint set by the cosmic microwave background (CMB) on the observed structural and dynamical characteristics of galaxies, as deduced from dust continuum and CO-line imaging at high redshifts. As the CMB temperature rises in the distant Universe, the ensuing thermal equilibrium between the CMB and the cold dust and H 2 gas progressively erases all spatial and spectral contrasts between their brightness distributions and the CMB. For high-redshift galaxies, this strongly biases the recoverable H 2 gas and dust mass distributions, scale lengths, gas velocity fields and dynamical mass estimates. This limitation is unique to millimetre/submillimetre wavelengths and unlike its known effect on the global dust continuum and molecular line emission of galaxies, it cannot be addressed simply. We nevertheless identify a unique signature of CMB-affected continuum brightness distributions, namely an increasing rather than diminishing contrast between such brightness distributions and the CMB when the cold dust in distant galaxies is imaged at frequencies beyond the Raleigh–Jeans limit. For the molecular gas tracers, the same effect makes the atomic carbon lines maintain a larger contrast than the CO lines against the CMB.

scholarly journals Study of the Gas Kinematics in the Center of the Barred Spiral Galaxy NGC 4258.

1996 ◽  
Vol 157 ◽  
pp. 164-167
Author(s):  
S. N. Dodonov
Keyword(s):  
Spiral Galaxy ◽  
Spatial Sampling ◽  
Kinematic Structure ◽  
Gas Kinematics ◽  
Barred Spiral Galaxy ◽  
Integral Field Spectrograph ◽  
Integral Field

AbstractIntegral Field Spectrograph observations of southeast (SE) gas outflow in the center (11×13 arcsec) of NGC 4258 with spatial sampling 0.6 and 1.2 arcsec were made with the 6-m Telescope. Reconstructed spatial and kinematic structure of the SE outflow from 20-30 pc to 200-220 pc are presented.

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