scholarly journals Hubble Space Telescope Observations of [O III] Emission in Nearby QSO2s: Physical Properties of the Ionised Outflows

2020 ◽  
Author(s):  
Anna Trindade Falcão ◽  
S B Kraemer ◽  
T C Fischer ◽  
D M Crenshaw ◽  
M Revalski ◽  
...  
Keyword(s):  
Physical Properties ◽  
Emission Line ◽  
Hubble Space Telescope ◽  
Radial Distance ◽  
Flow Rates ◽  
Space Telescope ◽  
Bolometric Luminosity ◽  
Mass Outflow ◽  
Peak Outflow ◽  
Imaging Spectrograph

Abstract We use Hubble Space Telescope (HST)/ Space Telescope Imaging Spectrograph (STIS) long-slit G430M and G750M spectra to analyse the extended [O III] λ5007 emission in a sample of twelve nearby (z >0.12) luminous (Lbol > 1.6 × 1045 erg s−1) QSO2s. The purpose of the study is to determine the properties of the mass outflows of ionised gas and their role in AGN feedback. We measure fluxes and velocities as functions of radial distances. Using Cloudy models and ionising luminosities derived from [O III] λ5007, we are able to estimate the densities for the emission-line gas. From these results, we derive masses of [O III]-emitting gas, mass outflow rates, kinetic energies, kinetic luminosities, momenta and momentum flow rates as a function of radial distance for each of the targets. For the sample, masses are several times 103M⊙ − 107M⊙ and peak outflow rates are 9.3 × 10−3M⊙ yr−1 to 10.3 M⊙ yr−1. The peak kinetic luminosities are 3.4 × 10−8 to 4.9 × 10−4 of the bolometric luminosity, which does not approach the 5.0 × 10−3 - 5.0 × 10−2 range required by some models for efficient feedback. For Mrk 34, which has the largest kinetic luminosity of our sample, in order to produce efficient feedback there would have to be 10 times more [O III]-emitting gas than we detected at its position of maximum kinetic luminosity. Three targets show extended [O III] emission, but compact outflow regions. This may be due to different mass profiles or different evolutionary histories.

HST observations of [O III] emission in nearby QSO2s: Physical properties of the outflows

2020 ◽  
Vol 15 (S359) ◽  
pp. 269-271
Author(s):  
Anna Trindade Falcao ◽  
S. B. Kraemer ◽  
T. C. Fischer ◽  
D. M. Crenshaw ◽  
M. Revalski ◽  
...  
Keyword(s):  
Physical Properties ◽  
Emission Line ◽  
Radial Distance ◽  
Space Telescope ◽  
X Ray ◽  
Medium Resolution ◽  
Mass Outflow ◽  
Imaging Spectrograph

AbstractWe used Space Telescope Imaging Spectrograph (STIS) long slit medium-resolution G430M and G750M spectra to analyze the extended [O III] λ5007 emission in a sample of twelve QSO2s from Reyes et al. (2008). The purpose of the study was to determine the properties of the mass outflows and their role in AGN feedback. We measured fluxes and velocities as functions of deprojected radial distances. Using photoionization models and ionizing luminosities derived from [O III], we were able to estimate the densities for the emission-line gas. From these results, we derived masses, mass outflow rates, kinetic energies and kinetic luminosity rates as a function of radial distance for each of the targets. Masses are several times 103 - 107 solar masses, which are comparable to values determined from a recent photoionization study of Mrk 34 (Revalski). Additionally, we are studying the possible role of X-ray winds in these QSO2s.

scholarly journals Quantifying the AGN-driven outflows in ULIRGs (QUADROS) IV: HST/STIS spectroscopy of the sub-kpc warm outflow in F14394+5332

2019 ◽  
Vol 488 (2) ◽  
pp. 1813-1821 ◽  
Author(s):  
C Tadhunter ◽  
L Holden ◽  
C Ramos Almeida ◽  
D Batcheldor
Keyword(s):  
Hubble Space Telescope ◽  
Outer Part ◽  
Ionization State ◽  
Space Telescope ◽  
High Ionization ◽  
Mass Outflow ◽  
Outflow Region ◽  
First Time ◽  
Imaging Spectrograph ◽  
Luminous Infrared Galaxy

ABSTRACT Considerable uncertainties remain about the nature of warm, AGN-driven outflows and their impact on the evolution of galaxies. This is because the outflows are often unresolved in ground-based observations. As part of a project to study the AGN outflows in some of the most rapidly evolving galaxies in the local Universe, here we present Hubble Space Telescope (HST)/Space Telescope Imaging Spectrograph (STIS) observations of F14394+5332E that resolve the sub-kpc warm outflow for the first time in an ultra-luminous infrared galaxy. The observations reveal a compact, high-ionization outflow region (rmax ∼ 0.9 kpc) set in a more extensive (rmax ∼ 1.4 kpc) halo that is kinematically quiescent and has a lower ionization state. A large line width (600 < FWHM < 1500 km s−1) is measured throughout the outflow region, and the outflowing gas shows a steep velocity gradient with radius, with the magnitude of the blueshifted velocities increasing from ∼500 to 1800 km s−1 from the inner to the outer part of the outflow. We interpret the observations in terms of the local acceleration, and hydrodynamic destruction, of dense clouds as they are swept up in a hot, low-density wind driven by the AGN. We discuss the implications for measuring the mass outflow rates and kinetic powers for the AGN-driven outflows in such objects.

scholarly journals Mass outflow of the X-ray emission line gas in NGC 4151

2020 ◽  
Vol 15 (S359) ◽  
pp. 131-135
Author(s):  
S. B. Kraemer ◽  
T. J. Turner ◽  
D. M. Crenshaw ◽  
H. R. Schmitt ◽  
M. Revalski ◽  
...  
Keyword(s):  
Emission Line ◽  
Total Mass ◽  
High Energy ◽  
Model Parameters ◽  
Zeroth Order ◽  
Space Telescope ◽  
X Ray ◽  
Ngc 4151 ◽  
Outflow Rate ◽  
Mass Outflow

AbstractWe have analyzed Chandra/High Energy Transmission Grating spectra of the X-ray emission line gas in the Seyfert galaxy NGC 4151. The zeroth-order spectral images show extended H- and He-like O and Ne, up to a distance r ˜ 200 pc from the nucleus. Using the 1st-order spectra, we measure an average line velocity ˜230 km s–1, suggesting significant outflow of X-ray gas. We generated Cloudy photoionization models to fit the 1st-order spectra; the fit required three distinct emission-line components. To estimate the total mass of ionized gas (M) and the mass outflow rates, we applied the model parameters to fit the zeroth-order emission-line profiles of Ne IX and Ne X. We determined an M ≍ 5.4 × 105Mʘ. Assuming the same kinematic profile as that for the [O III] gas, derived from our analysis of Hubble Space Telescope/Space Telescope Imaging Spectrograph spectra, the peak X-ray mass outflow rate is approximately 1.8 Mʘ yr–1, at r ˜ 150 pc. The total mass and mass outflow rates are similar to those determined using [O III], implying that the X-ray gas is a major outflow component. However, unlike the optical outflows, the X-ray emitting mass outflow rate does not drop off at r > 100pc, which suggests that it may have a greater impact on the host galaxy.

Spitzer and Hubble Space Telescope Constraints on the Physical Properties of the z  ~ 7 Galaxy Strongly Lensed by A2218

2004 ◽  
Vol 618 (1) ◽  
pp. L5-L8 ◽  
Author(s):  
E. Egami ◽  
J.-P. Kneib ◽  
G. H. Rieke ◽  
R. S. Ellis ◽  
J. Richard ◽  
...  
Keyword(s):  
Physical Properties ◽  
Hubble Space Telescope ◽  
Space Telescope

scholarly journals Current Status of the Astrometric Capabilities of the Hubble Space Telescope Fine Guidance Sensors

1991 ◽  
Vol 127 ◽  
pp. 68-76
Author(s):  
W.H. Jefferys ◽  
G.F. Benedict ◽  
R.L. Duncombe ◽  
O.G. Franz ◽  
L.W. Fredrick ◽  
...  
Keyword(s):  
Optical System ◽  
Reference Frames ◽  
Optical Axis ◽  
Hubble Space Telescope ◽  
Current Knowledge ◽  
Spherical Aberration ◽  
Radial Distance ◽  
Current Status ◽  
Space Telescope ◽  
Wavefront Error

AbstractThe Fine Guidance Sensors (FGSs) are the instrument of choice for most astrometric measurements with the Hubble Space Telescope (HST). The observed amount of spherical aberration in the Ritchey Chretien optical system does not affect positional measurements with perfectly aligned FGSs because they are interferometers. The FGSs combine wavefronts from points in the exit pupil with other points which are at the same radial distance from the optical axis. Asymmetric aberrations such as coma and astigmatism do affect the measured positions. The current knowledge of the HST wavefront error, the FGS operation and the implications for milliarcsecond relative astrometry are discussed. It is still planned to use the HST to tie the HIPPARCOS and VLBI Reference Frames together at the few milliarcsecond level.

scholarly journals Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters

2020 ◽  
Vol 493 (4) ◽  
pp. 5120-5130 ◽  
Author(s):  
Michael V Maseda ◽  
Roland Bacon ◽  
Daniel Lam ◽  
Jorryt Matthee ◽  
Jarle Brinchmann ◽  
...  
Keyword(s):  
Physical Properties ◽  
Emission Line ◽  
Equivalent Width ◽  
Production Efficiency ◽  
Hubble Space Telescope ◽  
Stellar Populations ◽  
Photon Production ◽  
Efficient Production ◽  
Number Counts ◽  
Lower Luminosity

ABSTRACT While low-luminosity galaxies dominate number counts at all redshifts, their contribution to cosmic reionization is poorly understood due to a lack of knowledge of their physical properties. We isolate a sample of 35 z ≈ 4–5 continuum-faint Lyman-α emitters from deep VLT/MUSE spectroscopy and directly measure their H α emission using stacked Spitzer/IRAC Ch. 1 photometry. Based on Hubble Space Telescope imaging, we determine that the average UV continuum magnitude is fainter than −16 (≈ 0.01 L⋆), implying a median Lyman-α equivalent width of 259 Å. By combining the H α measurement with the UV magnitude, we determine the ionizing photon production efficiency, ξion, a first for such faint galaxies. The measurement of log10 (ξion [Hz erg−1]) = 26.28 ($^{+0.28}_{-0.40}$) is in excess of literature measurements of both continuum- and emission line-selected samples, implying a more efficient production of ionizing photons in these lower luminosity, Lyman-α-selected systems. We conclude that this elevated efficiency can be explained by stellar populations with metallicities between 4 × 10−4 and 0.008, with light-weighted ages less than 3 Myr.

scholarly journals [ITAL]Hubble Space Telescope[/ITAL] Space Telescope Imaging Spectrograph Imaging of the Host Galaxy of GRB 980425/SN 1998[CLC]bw[/CLC]

2000 ◽  
Vol 542 (2) ◽  
pp. L89-L93 ◽  
Author(s):  
J. U. Fynbo ◽  
S. Holland ◽  
M. I. Andersen ◽  
B. Thomsen ◽  
J. Hjorth ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Host Galaxy ◽  
Space Telescope ◽  
Imaging Spectrograph

Space Telescope Imaging Spectrograph Spectroscopy of the Emission‐Line Gas in the Nuclei of Nearby FR‐I Galaxies

2003 ◽  
Vol 148 (2) ◽  
pp. 419-472 ◽  
Author(s):  
Jacob Noel‐Storr ◽  
Stefi A. Baum ◽  
Gijs Verdoes Kleijn ◽  
Roeland P. van der Marel ◽  
Christopher P. O’Dea ◽  
...  
Keyword(s):  
Emission Line ◽  
Space Telescope ◽  
Imaging Spectrograph

scholarly journals The Interstellar Abundance of Lead: Experimental Oscillator Strengths for Pb ii λ1203 and λ1433 and New Detections of Pb ii in the Interstellar Medium

2015 ◽  
Vol 11 (A29A) ◽  
Author(s):  
A. M. Ritchey ◽  
N. Heidarian ◽  
R. E. Irving ◽  
S. R. Federman ◽  
D. G. Ellis ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Hubble Space Telescope ◽  
Oscillator Strengths ◽  
Interstellar Gas ◽  
Lifetime Measurements ◽  
Space Telescope ◽  
Interstellar Grains ◽  
Imaging Spectrograph ◽  
Theoretical Results ◽  
Beam Foil

AbstractWe present the first experimentally determined oscillator strengths for the Pb ii transitions at 1203.6 Å and 1433.9 Å, obtained from lifetime measurements made using beam-foil techniques. We also present new detections of these lines in the interstellar medium from an analysis of archival spectra acquired by the Space Telescope Imaging Spectrograph onboard the Hubble Space Telescope. Our observations of the Pb ii λ1203 line represent the first detection of this transition in interstellar gas. Our experimental f-values for the Pb ii λ1203 and λ1433 transitions are consistent with recent theoretical results, including our own relativistic calculations, but are significantly smaller than previous values based on older calculations. Our new f-value for Pb ii λ1433 (0.321 ± 0.034) yields an increase in the interstellar abundance of Pb of 0.43 dex over estimates based on the f-value listed by Morton. With our revised f-values, and with our new detections of Pb ii λ1203 and λ1433, we find that the depletion of Pb onto interstellar grains is not nearly as severe as previously thought, and is very similar to the depletions seen for elements such as Zn and Sn, which have similar condensation temperatures.

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