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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.02961">arXiv:2212.02961</a> <span> [<a href="https://arxiv.org/pdf/2212.02961">pdf</a>, <a href="https://arxiv.org/format/2212.02961">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245047">10.1051/0004-6361/202245047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supermassive Black Hole Winds in X-rays: SUBWAYS. II. HST UV spectroscopy of winds at intermediate redshifts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mehdipour%2C+M">M. Mehdipour</a>, <a href="/search/astro-ph?searchtype=author&query=Kriss%2C+G+A">G. A. Kriss</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Matzeu%2C+G+A">G. A. Matzeu</a>, <a href="/search/astro-ph?searchtype=author&query=Gaspari%2C+M">M. Gaspari</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Behar%2C+E">E. Behar</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Cappi%2C+M">M. Cappi</a>, <a href="/search/astro-ph?searchtype=author&query=Chartas%2C+G">G. Chartas</a>, <a href="/search/astro-ph?searchtype=author&query=Costantini%2C+E">E. Costantini</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">M. Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+B">B. De Marco</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+A">A. De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">J. P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Gianolli%2C+V+E">V. E. Gianolli</a>, <a href="/search/astro-ph?searchtype=author&query=Giustini%2C+M">M. Giustini</a>, <a href="/search/astro-ph?searchtype=author&query=Kaastra%2C+J+S">J. S. Kaastra</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+A+R">A. R. King</a>, <a href="/search/astro-ph?searchtype=author&query=Krongold%2C+Y">Y. Krongold</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Longinotti%2C+A+L">A. L. Longinotti</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.02961v1-abstract-short" style="display: inline;"> We present a UV spectroscopic study of ionized outflows in 21 active galactic nuclei (AGN), observed with the HST. The targets of the SUBWAYS sample were selected with the aim to probe the parameter space of the underexplored AGN between the local Seyfert galaxies and the luminous quasars at high redshifts. Our targets, spanning redshifts of 0.1-0.4 and bolometric luminosities (L_bol) of 10^45-10^… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02961v1-abstract-full').style.display = 'inline'; document.getElementById('2212.02961v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.02961v1-abstract-full" style="display: none;"> We present a UV spectroscopic study of ionized outflows in 21 active galactic nuclei (AGN), observed with the HST. The targets of the SUBWAYS sample were selected with the aim to probe the parameter space of the underexplored AGN between the local Seyfert galaxies and the luminous quasars at high redshifts. Our targets, spanning redshifts of 0.1-0.4 and bolometric luminosities (L_bol) of 10^45-10^46 erg/s, have been observed with a large multi-wavelength campaign. Here, we model the UV spectra and look for different types of AGN outflows. We find that 60% of our targets show a presence of outflowing H I absorption, while 40% exhibit ionized outflows seen as absorption by either C IV, N V, or O VI. This is comparable to the occurrence of ionized outflows seen in the local Seyfert galaxies. All UV absorption lines in the sample are relatively narrow, with outflow velocities reaching up to -3300 km/s. We did not detect any UV counterparts to the X-ray ultra-fast outflows (UFOs), most likely due to their being too highly ionized. However, all SUBWAYS targets with an X-ray UFO demonstrate the presence of UV outflows at lower velocities. We find significant correlations between the column density (N) of the UV ions and L_bol of the AGN, with N of H I decreasing with L_bol, while N of O VI is increasing with L_bol. This is likely to be a photoionization effect, where toward higher AGN luminosities, the wind becomes more ionized, resulting in less absorption by neutral or low-ionization ions and more absorption by high-ionization ions. In addition, we find that N of the UV ions decreases as their outflow velocity increases. This may be explained by a mechanical power that is evacuating the UV-absorbing medium. Our observed relations are consistent with multiphase AGN feeding and feedback simulations indicating that a combination of both radiative and mechanical processes are in play. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02961v1-abstract-full').style.display = 'none'; document.getElementById('2212.02961v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics (A&A), 22 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.04406">arXiv:1805.04406</a> <span> [<a href="https://arxiv.org/pdf/1805.04406">pdf</a>, <a href="https://arxiv.org/ps/1805.04406">ps</a>, <a href="https://arxiv.org/format/1805.04406">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aaa95d">10.3847/1538-4357/aaa95d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evolution of the Outflows in NGC 3516 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Parvaresh%2C+R">Rozhin Parvaresh</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. Michael Crenshaw</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1805.04406v1-abstract-short" style="display: inline;"> We analyze the 2011 HST/COS spectrum of the Seyfert 1 galaxy NGC 3516, which demonstrates clear changes in one of the intrinsic absorption troughs (component 5), slight evidence of change in a second trough (component 6), and the appearance of a new absorption trough (component 9). We interpret both the changes and the appearance of the new trough as bulk motion across the line of sight. The impli… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.04406v1-abstract-full').style.display = 'inline'; document.getElementById('1805.04406v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.04406v1-abstract-full" style="display: none;"> We analyze the 2011 HST/COS spectrum of the Seyfert 1 galaxy NGC 3516, which demonstrates clear changes in one of the intrinsic absorption troughs (component 5), slight evidence of change in a second trough (component 6), and the appearance of a new absorption trough (component 9). We interpret both the changes and the appearance of the new trough as bulk motion across the line of sight. The implied lower limit on the transverse velocity of component 5 is 360 km/s, compared to the earlier 2001 HST/STIS spectrum, while the lower limits for components 6 and 9 are 920 km/s, based on 2009 FUSE data. Component 5 also exhibits a shift in velocity centroid. This is only the second known case of this behavior in a Seyfert galaxy. Due to the high quality of the HST/COS spectrum, we identify a previously undetected trough due to an excited state of Si II for component 1. In combination with the resonance trough of Si II and photoionization modeling, we directly determine the distance of the component 1 outflow to be 67.2 pc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.04406v1-abstract-full').style.display = 'none'; document.getElementById('1805.04406v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2018, ApJ, 854, 166D </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.05060">arXiv:1509.05060</a> <span> [<a href="https://arxiv.org/pdf/1509.05060">pdf</a>, <a href="https://arxiv.org/ps/1509.05060">ps</a>, <a href="https://arxiv.org/format/1509.05060">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/808/1/94">10.1088/0004-637X/808/1/94 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Determining the Locations of Dust Sources in FeLoBAL Quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Wasik%2C+B">Branden Wasik</a>, <a href="/search/astro-ph?searchtype=author&query=Holtzclaw%2C+C+L">Christin L. Holtzclaw</a>, <a href="/search/astro-ph?searchtype=author&query=Yenerall%2C+D">David Yenerall</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+M">Manuel Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Arav%2C+N">Nahum Arav</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+D">Daniel Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Moe%2C+M">Max Moe</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">Luis C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Dutton%2C+S+H">S. Harper Dutton</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.05060v1-abstract-short" style="display: inline;"> We conduct a spectroscopic search of quasars observed by the Sloan Digital Sky Survey (SDSS) with broad absorption line (BAL) troughs due to Mg II and troughs due to Fe II that simultaneously exhibit strong Balmer narrow emission lines (NELs). We find that in a redshift range of 0.4 less than or equal to z less than or equal to 0.9 approximately 23 of the 70 Mg II BALs and 4 of a subset of 15 Fe I… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.05060v1-abstract-full').style.display = 'inline'; document.getElementById('1509.05060v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.05060v1-abstract-full" style="display: none;"> We conduct a spectroscopic search of quasars observed by the Sloan Digital Sky Survey (SDSS) with broad absorption line (BAL) troughs due to Mg II and troughs due to Fe II that simultaneously exhibit strong Balmer narrow emission lines (NELs). We find that in a redshift range of 0.4 less than or equal to z less than or equal to 0.9 approximately 23 of the 70 Mg II BALs and 4 of a subset of 15 Fe II BALs exhibit strong Balmer emission. We also find significant fractions of Mg II BALs (approximately 23%) and those Mg II BALs with Fe II troughs (approximately 27%) have strong continuum reddening, E(B - V) greater than or equal to 0.1. From measurements of the Balmer decrement in three objects, we find similarly significant reddening of the NEL region in three of the four objects; the NELs in the fourth object are not measurable. We also include one object in this study not taken from the SDSS sample that shows Fe II absorption and strong narrow emission, but due to measurement uncertainty and low continuum reddening the comparison is consistent but inconclusive. We find a trend in both the Mg II and Fe II BAL samples between the NEL reddening and continuum reddening. Because the narrow line reddening is consistent with the continuum reddening in every object in the two SDSS samples, it suggests that the reddening sources in these objects likely exist at larger radial distances than the narrow line regions from the central nucleus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.05060v1-abstract-full').style.display = 'none'; document.getElementById('1509.05060v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">40 manuscript pages, accepted in ApJ (July)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 808, 94, 2015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1206.7026">arXiv:1206.7026</a> <span> [<a href="https://arxiv.org/pdf/1206.7026">pdf</a>, <a href="https://arxiv.org/ps/1206.7026">ps</a>, <a href="https://arxiv.org/format/1206.7026">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/750/2/143">10.1088/0004-637X/750/2/143 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BAL Outflow Contribution to AGN Feedback: Frequency of S iv Outflows in the SDSS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Arav%2C+N">Nahum Arav</a>, <a href="/search/astro-ph?searchtype=author&query=Aoki%2C+K">Kentaro Aoki</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+A">Ashlee Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Laughlin%2C+C">Courtney Laughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Edmonds%2C+D">Doug Edmonds</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+M">Manuel Bautista</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1206.7026v1-abstract-short" style="display: inline;"> We present a study of Broad Absorption Line (BAL) quasar outflows that show S IV ?1063 and S IV* ?1073 troughs. The fractional abundance of S IV and C IV peak at similar value of the ionization parameter, implying that they arise from the same physical component of the outflow. Detection of the S IV* troughs will allow us to determine the distance to this gas with higher resolution and higher sign… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.7026v1-abstract-full').style.display = 'inline'; document.getElementById('1206.7026v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1206.7026v1-abstract-full" style="display: none;"> We present a study of Broad Absorption Line (BAL) quasar outflows that show S IV ?1063 and S IV* ?1073 troughs. The fractional abundance of S IV and C IV peak at similar value of the ionization parameter, implying that they arise from the same physical component of the outflow. Detection of the S IV* troughs will allow us to determine the distance to this gas with higher resolution and higher signal-to-noise spectra, therefore providing the distance and energetics of the ubiquitous C IV BAL outflows. In our bright sample of 156 SDSS quasars 14% show C IV and 1.9% S IV troughs, which is consistent with a fainter magnitude sample with twice as many objects. One object in the fainter sample shows evidence of a broad S IV trough without any significant trough present from the excited state line, which implies that this outflow could be at a distance of several kpc. Given the fractions of C IV and S IV, we establish firm limits on the global covering factor on S IV that ranges from 2.8% to 21% (allowing for the k-correction). Comparison of the expected optical depth for these ions with their detected percentage suggests that these species arise from common outflows with a covering factor closer to the latter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.7026v1-abstract-full').style.display = 'none'; document.getElementById('1206.7026v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 June, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in ApJ (2012 ApJ, 750, 143)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2012 ApJ, 750, 143 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1204.2258">arXiv:1204.2258</a> <span> [<a href="https://arxiv.org/pdf/1204.2258">pdf</a>, <a href="https://arxiv.org/ps/1204.2258">ps</a>, <a href="https://arxiv.org/format/1204.2258">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/751/2/84">10.1088/0004-637X/751/2/84 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observations of Outflowing UV Absorbers in NGC 4051 with the Cosmic Origins Spectrograph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. M. Crenshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">J. P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+T+J">T. J. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Lobban%2C+A+P">A. P. Lobban</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+L">L. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+J+N">J. N. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Fischer%2C+T+C">T. C. Fischer</a>, <a href="/search/astro-ph?searchtype=author&query=Braito%2C+V">V. Braito</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1204.2258v1-abstract-short" style="display: inline;"> We present new Hubble Space Telescope (HST)/Cosmic Origins Spectrograph observations of the Narrow-Line Seyfert 1 galaxy NGC 4051. These data were obtained as part of a coordinated observing program including X-ray observations with the Chandra/High Energy Transmission Grating (HETG) Spectrometer and Suzaku. We detected nine kinematic components of UV absorption, which were previously identified u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1204.2258v1-abstract-full').style.display = 'inline'; document.getElementById('1204.2258v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1204.2258v1-abstract-full" style="display: none;"> We present new Hubble Space Telescope (HST)/Cosmic Origins Spectrograph observations of the Narrow-Line Seyfert 1 galaxy NGC 4051. These data were obtained as part of a coordinated observing program including X-ray observations with the Chandra/High Energy Transmission Grating (HETG) Spectrometer and Suzaku. We detected nine kinematic components of UV absorption, which were previously identified using the HST/Space Telescope Imaging Spectrograph. None of the absorption components showed evidence for changes in column density or profile within the \sim 10 yr between the STIS and COS observations, which we interpret as evidence of 1) saturation, for the stronger components, or 2) very low densities, i.e., n_H < 1 cm^-3, for the weaker components. After applying a +200 km s^-1 offset to the HETG spectrum, we found that the radial velocities of the UV absorbers lay within the O VII profile. Based on photoionization models, we suggest that, while UV components 2, 5 and 7 produce significant O VII absorption, the bulk of the X-ray absorption detected in the HETG analysis occurs in more highly ionized gas. Moreover, the mass loss rate is dominated by high ionization gas which lacks a significant UV footprint. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1204.2258v1-abstract-full').style.display = 'none'; document.getElementById('1204.2258v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 April, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">41 pages, 10 Figures; accepted for publication in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1106.2084">arXiv:1106.2084</a> <span> [<a href="https://arxiv.org/pdf/1106.2084">pdf</a>, <a href="https://arxiv.org/ps/1106.2084">ps</a>, <a href="https://arxiv.org/format/1106.2084">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Galactic Scale Absorption Outflow in the Low Luminosity Quasar IRAS~F04250-5718: HST/COS Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Edmonds%2C+D">Doug Edmonds</a>, <a href="/search/astro-ph?searchtype=author&query=Borguet%2C+B">Benoit Borguet</a>, <a href="/search/astro-ph?searchtype=author&query=Arav%2C+N">Nahum Arav</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Penton%2C+S">Steve Penton</a>, <a href="/search/astro-ph?searchtype=author&query=Kriss%2C+G+A">Gerard A. Kriss</a>, <a href="/search/astro-ph?searchtype=author&query=Korista%2C+K">Kirk Korista</a>, <a href="/search/astro-ph?searchtype=author&query=Costantini%2C+E">Elisa Costantini</a>, <a href="/search/astro-ph?searchtype=author&query=Steenbrugge%2C+K">Katrien Steenbrugge</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Serrano%2C+J+I">J. Ignacio Gonzalez-Serrano</a>, <a href="/search/astro-ph?searchtype=author&query=Aoki%2C+K">Kentaro Aoki</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+M">Manuel Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Behar%2C+E">Ehud Behar</a>, <a href="/search/astro-ph?searchtype=author&query=Benn%2C+C">Chris Benn</a>, <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. Micheal Crenshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+J">John Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Gabel%2C+J">Jack Gabel</a>, <a href="/search/astro-ph?searchtype=author&query=Kaastra%2C+J">Jelle Kaastra</a>, <a href="/search/astro-ph?searchtype=author&query=Moe%2C+M">Maxwell Moe</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+J">Jennifer Scott</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1106.2084v1-abstract-short" style="display: inline;"> We present absorption line analysis of the outflow in the quasar IRAS F04250-5718. Far-ultraviolet data from the Cosmic Origins Spectrograph onboard the Hubble Space Telescope reveal intrinsic narrow absorption lines from high ionization ions (e.g., C IV, N V, and O VI) as well as low ionization ions (e.g., C II and Si III). We identify three kinematic components with central velocities ranging fr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.2084v1-abstract-full').style.display = 'inline'; document.getElementById('1106.2084v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1106.2084v1-abstract-full" style="display: none;"> We present absorption line analysis of the outflow in the quasar IRAS F04250-5718. Far-ultraviolet data from the Cosmic Origins Spectrograph onboard the Hubble Space Telescope reveal intrinsic narrow absorption lines from high ionization ions (e.g., C IV, N V, and O VI) as well as low ionization ions (e.g., C II and Si III). We identify three kinematic components with central velocities ranging from ~-50 to ~-230 km/s. Velocity dependent, non-black saturation is evident from the line profiles of the high ionization ions. From the non-detection of absorption from a metastable level of C II, we are able to determine that the electron number density in the main component of the outflow is < 30 per cubic cm. Photoionization analysis yields an ionization parameter log U ~ -1.6 +/- 0.2, which accounts for changes in the metallicity of the outflow and the shape of the incident spectrum. We also consider solutions with two ionization parameters. If the ionization structure of the outflow is due to photoionization by the active galactic nucleus, we determine that the distance to this component from the central source is > 3 kpc. Due to the large distance determined for the main kinematic component, we discuss the possibility that this outflow is part of a galactic wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.2084v1-abstract-full').style.display = 'none'; document.getElementById('1106.2084v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1101.4340">arXiv:1101.4340</a> <span> [<a href="https://arxiv.org/pdf/1101.4340">pdf</a>, <a href="https://arxiv.org/ps/1101.4340">ps</a>, <a href="https://arxiv.org/format/1101.4340">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/pasj/63.sp2.S457">10.1093/pasj/63.sp2.S457 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Outflow in Overlooked Luminous Quasar: Subaru Observations of AKARI J1757+5907 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aoki%2C+K">Kentaro Aoki</a>, <a href="/search/astro-ph?searchtype=author&query=Oyabu%2C+S">Shinki Oyabu</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Arav%2C+N">Nahum Arav</a>, <a href="/search/astro-ph?searchtype=author&query=Edmonds%2C+D">Doug Edmonds</a>, <a href="/search/astro-ph?searchtype=author&query=Korista%2C+K+T">Kirk T. Korista</a>, <a href="/search/astro-ph?searchtype=author&query=Matsuhara%2C+H">Hideo Matsuhara</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1101.4340v1-abstract-short" style="display: inline;"> We present Subaru observations of the newly discovered luminous quasar AKARI J1757+5907, which shows an absorption outflow in its spectrum. The absorption consists of 9 distinct troughs, and our analysis focuses on the troughs at ~ -1000$ km s^{-1} for which we can measure accurate column densities of He I*, Fe II and Mg II. We use photoionization models to constrain the ionization parameter, tota… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.4340v1-abstract-full').style.display = 'inline'; document.getElementById('1101.4340v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1101.4340v1-abstract-full" style="display: none;"> We present Subaru observations of the newly discovered luminous quasar AKARI J1757+5907, which shows an absorption outflow in its spectrum. The absorption consists of 9 distinct troughs, and our analysis focuses on the troughs at ~ -1000$ km s^{-1} for which we can measure accurate column densities of He I*, Fe II and Mg II. We use photoionization models to constrain the ionization parameter, total hydrogen column density, and the number density of the outflowing gas. These constraints yield lower limits for the distance, mass flow rate and kinetic luminosity for the outflow of 3.7 kpc, 70 M_{sun} yr^{-1}, and 2.0 x 10^{43} ergs s^{-1}, respectively. Such mass flow rate value can contribute significantly to the metal enrichment of the intra-cluster medium. We find that this moderate velocity outflow is similar to those recently discovered in massive post-starburst galaxies. Finally, we describe the scientific potential of future observations targeting this object. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.4340v1-abstract-full').style.display = 'none'; document.getElementById('1101.4340v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in PASJ Subaru special issue in March 2011</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1011.4213">arXiv:1011.4213</a> <span> [<a href="https://arxiv.org/pdf/1011.4213">pdf</a>, <a href="https://arxiv.org/ps/1011.4213">ps</a>, <a href="https://arxiv.org/format/1011.4213">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/727/2/71">10.1088/0004-637X/727/2/71 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HST Observations of the Double-Peaked Emission Lines in the Seyfert Galaxy Markarian 78: Mass Outflows from a Single AGN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fischer%2C+T+C">T. C. Fischer</a>, <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. M. Crenshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Schmitt%2C+H+R">H. R. Schmitt</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotsky%2C+R+F">R. F. Mushotsky</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">J. P. Dunn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1011.4213v1-abstract-short" style="display: inline;"> Previous ground based observations of the Seyfert 2 galaxy Mrk 78 revealed a double set of emission lines, similar to those seen in several AGN from recent surveys. Are the double lines due to two AGN with different radial velocities in the same galaxy, or are they due to mass outflows from a single AGN?We present a study of the outflowing ionized gas in the resolved narrow-line region (NLR) of Mr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1011.4213v1-abstract-full').style.display = 'inline'; document.getElementById('1011.4213v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1011.4213v1-abstract-full" style="display: none;"> Previous ground based observations of the Seyfert 2 galaxy Mrk 78 revealed a double set of emission lines, similar to those seen in several AGN from recent surveys. Are the double lines due to two AGN with different radial velocities in the same galaxy, or are they due to mass outflows from a single AGN?We present a study of the outflowing ionized gas in the resolved narrow-line region (NLR) of Mrk 78 using observations from Space Telescope Imaging Spectrograph (STIS) and Faint Object Camera (FOC) aboard the Hubble Space Telescope(HST) as part of an ongoing project to determine the kinematics and geometries of active galactic nuclei (AGN) outflows. From the spectroscopic information, we deter- mined the fundamental geometry of the outflow via our kinematics modeling program by recreating radial velocities to fit those seen in four different STIS slit positions. We determined that the double emission lines seen in ground-based spectra are due to an asymmetric distribution of outflowing gas in the NLR. By successfully fitting a model for a single AGN to Mrk 78, we show that it is possible to explain double emission lines with radial velocity offsets seen in AGN similar to Mrk 78 without requiring dual supermassive black holes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1011.4213v1-abstract-full').style.display = 'none'; document.getElementById('1011.4213v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 7 figures (2 color), accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1006.0919">arXiv:1006.0919</a> <span> [<a href="https://arxiv.org/pdf/1006.0919">pdf</a>, <a href="https://arxiv.org/ps/1006.0919">ps</a>, <a href="https://arxiv.org/format/1006.0919">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/717/2/L98">10.1088/2041-8205/717/2/L98 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ionization Driven Fragmentation of Gas Outflows Responsible for FeLoBALs in Quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+M+A">Manuel A. Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1006.0919v1-abstract-short" style="display: inline;"> We show that time variations in the UV ionizing continuum of quasars, on scales of $\sim$1 year, affect the dynamic structure of the plasmas responsible for low ionization broad absorption lines. Variations of the ionizing continuum produce non-equilibrium photoionization conditions over a significant fraction of the absorbing clouds and supersonically moving ionization fronts. When the flux drops… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1006.0919v1-abstract-full').style.display = 'inline'; document.getElementById('1006.0919v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1006.0919v1-abstract-full" style="display: none;"> We show that time variations in the UV ionizing continuum of quasars, on scales of $\sim$1 year, affect the dynamic structure of the plasmas responsible for low ionization broad absorption lines. Variations of the ionizing continuum produce non-equilibrium photoionization conditions over a significant fraction of the absorbing clouds and supersonically moving ionization fronts. When the flux drops the contraction of the ionized region drives a supersonic cooling front towards the radiation source and a rarefaction wave in the opposite direction. The pressure imbalance is compensated by an increased speed of the cool gas relative to the front. When the flux recovers the cool gas is re-ionized and re-heated by a supersonic ionization front traveling away from the radiation source and a forward shock is created. The reheated clouds equilibrate to a temperature of $\sim 10^4$ K and are observed to have different radial velocities than the main cloud. Such fragmentation seems consistent with the multicomponent structure of troughs seen in some objects. The velocity differences measured among various components in the quasars QSO 2359--1241 and SDSS J0318--0600 can be reproduced by our model if strong magnetic fields ($\sim$10 mG) are present within the clouds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1006.0919v1-abstract-full').style.display = 'none'; document.getElementById('1006.0919v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 June, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">2 figure, accepted for publication in ApJ Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1003.0970">arXiv:1003.0970</a> <span> [<a href="https://arxiv.org/pdf/1003.0970">pdf</a>, <a href="https://arxiv.org/ps/1003.0970">ps</a>, <a href="https://arxiv.org/format/1003.0970">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/713/1/25">10.1088/0004-637X/713/1/25 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Distance to Multiple Kinematic Components of Quasar Outflows: VLT Observations of QSO 2359-1241 and SDSS J0318-0600 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+M+A">M. A. Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">J. P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Arav%2C+N">N. Arav</a>, <a href="/search/astro-ph?searchtype=author&query=Korista%2C+K+T">K. T. Korista</a>, <a href="/search/astro-ph?searchtype=author&query=Moe%2C+M">M. Moe</a>, <a href="/search/astro-ph?searchtype=author&query=Benn%2C+C">C. Benn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1003.0970v1-abstract-short" style="display: inline;"> Using high resolution VLT spectra, we study the multi-component outflow systems of two quasars exhibiting intrinsic Fe II absorption (QSO 2359-1241 and SDSS J0318-0600). From the extracted ionic column densities and using photoionization modeling we determine the gas density, total column density, and ionization parameter for several of the components. For each object the largest column density… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.0970v1-abstract-full').style.display = 'inline'; document.getElementById('1003.0970v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1003.0970v1-abstract-full" style="display: none;"> Using high resolution VLT spectra, we study the multi-component outflow systems of two quasars exhibiting intrinsic Fe II absorption (QSO 2359-1241 and SDSS J0318-0600). From the extracted ionic column densities and using photoionization modeling we determine the gas density, total column density, and ionization parameter for several of the components. For each object the largest column density component is also the densest, and all other components have densities of roughly 1/4 of that of the main component. We demonstrate that all the absorbers lie roughly at the same distance from the source. Further, we calculate the total kinetic luminosities and mass outflow rates of all components and show that these quantities are dominated by the main absorption component. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.0970v1-abstract-full').style.display = 'none'; document.getElementById('1003.0970v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 March, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0911.3896">arXiv:0911.3896</a> <span> [<a href="https://arxiv.org/pdf/0911.3896">pdf</a>, <a href="https://arxiv.org/ps/0911.3896">ps</a>, <a href="https://arxiv.org/format/0911.3896">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/709/2/611">10.1088/0004-637X/709/2/611 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Quasar Outflow Contribution to AGN Feedback: VLT Measurements of SDSS J0318-0600 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+M+A">Manuel A. Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Arav%2C+N">Nahum Arav</a>, <a href="/search/astro-ph?searchtype=author&query=Moe%2C+M">Maxwell Moe</a>, <a href="/search/astro-ph?searchtype=author&query=Korista%2C+K+T">Kirk T. Korista</a>, <a href="/search/astro-ph?searchtype=author&query=Costantini%2C+E">Elisa Costantini</a>, <a href="/search/astro-ph?searchtype=author&query=Benn%2C+C">Chris Benn</a>, <a href="/search/astro-ph?searchtype=author&query=Ellison%2C+S">Sara Ellison</a>, <a href="/search/astro-ph?searchtype=author&query=Edmonds%2C+D">Doug Edmonds</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0911.3896v1-abstract-short" style="display: inline;"> We present high spectral resolution VLT observations of the BAL quasar SDSS J0318-0600. This high quality data set allows us to extract accurate ionic column densities and determine an electron number density of n_e=10^3.3 +/- 0.2 cm^-3 for the main outflow absorption component. The heavily reddened spectrum of SDSS J0318-0600 requires purely silicate dust with a reddening curve characteristic o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.3896v1-abstract-full').style.display = 'inline'; document.getElementById('0911.3896v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0911.3896v1-abstract-full" style="display: none;"> We present high spectral resolution VLT observations of the BAL quasar SDSS J0318-0600. This high quality data set allows us to extract accurate ionic column densities and determine an electron number density of n_e=10^3.3 +/- 0.2 cm^-3 for the main outflow absorption component. The heavily reddened spectrum of SDSS J0318-0600 requires purely silicate dust with a reddening curve characteristic of predominately large grains, from which we estimate the bolometric luminosity. We carry out photoionization modeling to determine the total column density, ionization parameter and distance of the gas and find that the photionization models suggest abundances greater than solar. Due to the uncertainty in the location of the dust extinction, we arrive at two viable distances for the main ouflow component from the central source, 6 and 18 kpc, where we consider the 6 kpc location as somewhat more physically plausable. Assuming the canonical global covering of 20% for the outflow and a distance of 6 kpc, our analysis yields a mass flux of 120 M_sun yr^-1 and a kinetic luminosity that is ~0.1% of the bolometric luminosity of the object. Should the dust be part of the outflow, then these values are ~4x larger. The large mass flux and kinetic luminosity make this outflow a significant contributor to AGN feedback processes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.3896v1-abstract-full').style.display = 'none'; document.getElementById('0911.3896v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ, 57 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.709:611-631,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0911.0675">arXiv:0911.0675</a> <span> [<a href="https://arxiv.org/pdf/0911.0675">pdf</a>, <a href="https://arxiv.org/ps/0911.0675">ps</a>, <a href="https://arxiv.org/format/0911.0675">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/708/1/419">10.1088/0004-637X/708/1/419 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radial Velocity Offsets Due to Mass Outflows and Extinction in Active Galactic Nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. M. Crenshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Schmitt%2C+H+R">H. R. Schmitt</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R+F">R. F. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">J. P. Dunn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0911.0675v1-abstract-short" style="display: inline;"> We present a study of the radial velocity offsets between narrow emission lines and host galaxy lines (stellar absorption and H I 21-cm emission) in Seyfert galaxies with observed redshifts less than 0.043. We find that 35% of the Seyferts in the sample show [O III] emission lines with blueshifts with respect to their host galaxies exceeding 50 km/s, whereas only 6% show redshifts this large, in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.0675v1-abstract-full').style.display = 'inline'; document.getElementById('0911.0675v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0911.0675v1-abstract-full" style="display: none;"> We present a study of the radial velocity offsets between narrow emission lines and host galaxy lines (stellar absorption and H I 21-cm emission) in Seyfert galaxies with observed redshifts less than 0.043. We find that 35% of the Seyferts in the sample show [O III] emission lines with blueshifts with respect to their host galaxies exceeding 50 km/s, whereas only 6% show redshifts this large, in qualitative agreement with most previous studies. We also find that a greater percentage of Seyfert 1 galaxies show blueshifts than Seyfert 2 galaxies. Using HST/STIS spatially-resolved spectra of the Seyfert 2 galaxy NGC 1068 and the Seyfert 1 galaxy NGC 4151, we generate geometric models of their narrow-line regions (NLRs) and inner galactic disks, and show how these models can explain the blueshifted [O III] emission lines in collapsed STIS spectra of these two Seyferts. We conclude that the combination of mass outflow of ionized gas in the NLR and extinction by dust in the inner disk (primarily in the form of dust spirals) is primarily responsible for the velocity offsets in Seyfert galaxies. More exotic explanations are not needed. We discuss the implications of this result for the velocity offsets found in higher redshift AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.0675v1-abstract-full').style.display = 'none'; document.getElementById('0911.0675v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 7 figures, accepted for publication in the Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.708:419-426,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0807.0162">arXiv:0807.0162</a> <span> [<a href="https://arxiv.org/pdf/0807.0162">pdf</a>, <a href="https://arxiv.org/ps/0807.0162">ps</a>, <a href="https://arxiv.org/format/0807.0162">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/136/3/1201">10.1088/0004-6256/136/3/1201 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Intrinsic Absorption Properties in Active Galaxies Observed with the Far Ultraviolet Spectroscopic Explorer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. Michael Crenshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Trippe%2C+M+L">M. L. Trippe</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0807.0162v1-abstract-short" style="display: inline;"> In a continuing survey of active galactic nuclei observed by the Far Ultraviolet Spectroscopic Explorer, we provide a deeper analysis of intrinsic absorption features found in 35 objects. Our survey is for low-redshift and moderate-luminosity objects, mostly Seyfert galaxies. We find a strong correlation between maximum radial velocity and luminosity. We also examine the relationships between eq… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0807.0162v1-abstract-full').style.display = 'inline'; document.getElementById('0807.0162v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0807.0162v1-abstract-full" style="display: none;"> In a continuing survey of active galactic nuclei observed by the Far Ultraviolet Spectroscopic Explorer, we provide a deeper analysis of intrinsic absorption features found in 35 objects. Our survey is for low-redshift and moderate-luminosity objects, mostly Seyfert galaxies. We find a strong correlation between maximum radial velocity and luminosity. We also examine the relationships between equivalent width (EW), full width at half maximum, velocity: and continuum flux. The correlation between velocity and luminosity has been explored previously by Laor & Brandt, but at a significantly higher redshift and heavily weighted by broad absorption line quasars. We also have examined each object with multiple observations for variability in each of the aforementioned quantities, and have characterized the variation of EW with the continuum flux. In our survey, we find that variability of O VI lambda1032, lambda1038 is less common than of the UV doublets of CIV and N V seen at longer wavelengths, because the O VI absorption is usually saturated. Lyman beta absorption variability is more frequent. In a target-by-target examination we find that broad absorption line absorption and narrow absorption line absorbers are related in terms of maximum outflow velocity and luminosity, and both can be exhibited in similar luminosity objects. We also find one object that shows radial velocity change, seven objects that show equivalent width variability, and two objects that show either transverse velocity changes or a change in ionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0807.0162v1-abstract-full').style.display = 'none'; document.getElementById('0807.0162v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 July, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">56 pages, 23 figures, Accepted for AJ, 2008 May 19</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0706.3053">arXiv:0706.3053</a> <span> [<a href="https://arxiv.org/pdf/0706.3053">pdf</a>, <a href="https://arxiv.org/ps/0706.3053">ps</a>, <a href="https://arxiv.org/format/0706.3053">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/520644">10.1086/520644 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Survey of Intrinsic Absorption in Active Galaxies using the Far Ultraviolet Spectroscopic Explorer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. Michael Crenshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Gabel%2C+J+R">J. R. Gabel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0706.3053v1-abstract-short" style="display: inline;"> We present a survey of 72 Seyfert galaxies and quasars observed by the it Far Ultraviolet Spectroscopic Explorer (FUSE). We have determined that 72 of 253 available active galactic nuclei (AGN) targets are viable targets for detection of intrinsic absorption lines. We examined these spectra for signs of intrinsic absorption in the O VI doublet (lambda 1031.9, 1037.6) and Lyman beta (lambda 1025.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0706.3053v1-abstract-full').style.display = 'inline'; document.getElementById('0706.3053v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0706.3053v1-abstract-full" style="display: none;"> We present a survey of 72 Seyfert galaxies and quasars observed by the it Far Ultraviolet Spectroscopic Explorer (FUSE). We have determined that 72 of 253 available active galactic nuclei (AGN) targets are viable targets for detection of intrinsic absorption lines. We examined these spectra for signs of intrinsic absorption in the O VI doublet (lambda 1031.9, 1037.6) and Lyman beta (lambda 1025.7). The fraction of Seyfert 1 galaxies and low-redshift quasars at z < 0.15 that show evidence of intrinsic UV absorption is ~50%, which is slightly lower than Crenshaw et al. (1999) found (60%) based on a smaller sample of Seyfert 1 galaxies observed with the Hubble Space Telescope (HST). With this new fraction we find a global covering factor of the absorbing gas with respect to the central nucleus of ~0.4. Our survey is to date the largest searching for intrinsic UV absorption with high spectral resolution, and is the first step toward a more comprehensive study of intrinsic absorption in low-redshift AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0706.3053v1-abstract-full').style.display = 'none'; document.getElementById('0706.3053v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 June, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A higher resolution copy of the paper can be found at: http://www.chara.gsu.edu/~dunn/ms.ps</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J.134:1061-1071,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0704.3229">arXiv:0704.3229</a> <span> [<a href="https://arxiv.org/pdf/0704.3229">pdf</a>, <a href="https://arxiv.org/ps/0704.3229">ps</a>, <a href="https://arxiv.org/format/0704.3229">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/519015">10.1086/519015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Long Period, Massive Binaries HD 37366 and HD 54662: Potential Targets for Long Baseline Optical Interferometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boyajian%2C+T+S">T. S. Boyajian</a>, <a href="/search/astro-ph?searchtype=author&query=Gies%2C+D+R">D. R. Gies</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">J. P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Farrington%2C+C+D">C. D. Farrington</a>, <a href="/search/astro-ph?searchtype=author&query=Grundstrom%2C+E+D">E. D. Grundstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+W">W. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=McSwain%2C+M+V">M. V. McSwain</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+S+J">S. J. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Wingert%2C+D+W">D. W. Wingert</a>, <a href="/search/astro-ph?searchtype=author&query=Fullerton%2C+A+W">A. W. Fullerton</a>, <a href="/search/astro-ph?searchtype=author&query=Bolton%2C+C+T">C. T. Bolton</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0704.3229v1-abstract-short" style="display: inline;"> We present the results from an optical spectroscopic analysis of the massive stars HD 37366 and HD 54662. We find that HD 37366 is a double-lined spectroscopic binary with a period of 31.8187 +/- 0.0004 days, and HD 54662 is also a double lined binary with a much longer period of 557.8 +/- 0.3 days. The primary of HD 37366 is classified as O9.5 V, and it contributes approximately two-thirds of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0704.3229v1-abstract-full').style.display = 'inline'; document.getElementById('0704.3229v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0704.3229v1-abstract-full" style="display: none;"> We present the results from an optical spectroscopic analysis of the massive stars HD 37366 and HD 54662. We find that HD 37366 is a double-lined spectroscopic binary with a period of 31.8187 +/- 0.0004 days, and HD 54662 is also a double lined binary with a much longer period of 557.8 +/- 0.3 days. The primary of HD 37366 is classified as O9.5 V, and it contributes approximately two-thirds of the optical flux. The less luminous secondary is a broad-lined, early B-type main-sequence star. Tomographic reconstruction of the individual spectra of HD 37366 reveals absorption lines present in each component, enabling us to constrain the nature of the secondary and physical characteristics of both stars. Tomographic reconstruction was not possible for HD 54662; however, we do present mean spectra from our observations that show that the secondary component is approximately half as bright as the primary. The observed spectral energy distributions (SEDs) were fit with model SEDs and galactic reddening curves to determine the angular sizes of the stars. By assuming radii appropriate for their classifications, we determine distance ranges of 1.4 - 1.9 and 1.2 - 1.5 kpc for HD 37366 and HD 54662, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0704.3229v1-abstract-full').style.display = 'none'; document.getElementById('0704.3229v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 April, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 8 figures, Accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.664:1121-1129,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0603800">arXiv:astro-ph/0603800</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0603800">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0603800">ps</a>, <a href="https://arxiv.org/format/astro-ph/0603800">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/500961">10.1086/500961 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Internet Database of Ultraviolet Lightcurves for Seyfert Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">Jay P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+B">Brian Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Deo%2C+R+P">Rajesh P. Deo</a>, <a href="/search/astro-ph?searchtype=author&query=Farrington%2C+C">Chris Farrington</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+V">Varendra Das</a>, <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. Michael Crenshaw</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0603800v1-abstract-short" style="display: inline;"> Using the Multimission Archives at Space Telescope (MAST), we have extracted spectra and determined continuum light curves for 175 Seyfert Galaxies that have been observed with the International Ultraviolet Explorer (IUE) and the Faint Object Spectrograph (FOS) on the Hubble Space Telescope (HST). To obtain the light curves as a function of Julian Date, we used fix bins in the object's rest fram… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0603800v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0603800v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0603800v1-abstract-full" style="display: none;"> Using the Multimission Archives at Space Telescope (MAST), we have extracted spectra and determined continuum light curves for 175 Seyfert Galaxies that have been observed with the International Ultraviolet Explorer (IUE) and the Faint Object Spectrograph (FOS) on the Hubble Space Telescope (HST). To obtain the light curves as a function of Julian Date, we used fix bins in the object's rest frame, and measured small regions (between 30 and 60 Angstroms) of each spectrum's continuum flux in the range 1150 Angstroms to 3200 Angstroms. We provide access to the UV light curves and other basic information about the observations in tabular and graphical form via the Internet at http://www.chara.gsu.edu/PEGA/IUE/. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0603800v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0603800v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 March, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2006. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 9 figures, 3 tables, accepted for publication in April 2006 PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0305154">arXiv:astro-ph/0305154</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0305154">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0305154">ps</a>, <a href="https://arxiv.org/format/astro-ph/0305154">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/376792">10.1086/376792 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simultaneous UV and X-ray Spectroscopy of the Seyfert 1 Galaxy NGC 5548. I. Physical Conditions in the UV Absorbers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. M. Crenshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Gabel%2C+J+R">J. R. Gabel</a>, <a href="/search/astro-ph?searchtype=author&query=Kaastra%2C+J+S">J. S. Kaastra</a>, <a href="/search/astro-ph?searchtype=author&query=Steenbrugge%2C+K+C">K. C. Steenbrugge</a>, <a href="/search/astro-ph?searchtype=author&query=Brinkman%2C+A+C">A. C. Brinkman</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">J. P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=George%2C+I+M">I. M. George</a>, <a href="/search/astro-ph?searchtype=author&query=Liedahl%2C+D+A">D. A. Liedahl</a>, <a href="/search/astro-ph?searchtype=author&query=Paerels%2C+F+B+S">F. B. S. Paerels</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+T+J">T. J. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Yaqoob%2C+T">T. Yaqoob</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0305154v1-abstract-short" style="display: inline;"> We present new UV spectra of the nucleus of the Seyfert 1 galaxy NGC 5548, which we obtained with the Space Telescope Imaging Spectrograph at high spectral resolution, in conjunction with simultaneous Chandra X-ray Observatory spectra. Taking advantage of the low UV continuum and broad emission-line fluxes, we have determined that the deepest UV absorption component covers at least a portion of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0305154v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0305154v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0305154v1-abstract-full" style="display: none;"> We present new UV spectra of the nucleus of the Seyfert 1 galaxy NGC 5548, which we obtained with the Space Telescope Imaging Spectrograph at high spectral resolution, in conjunction with simultaneous Chandra X-ray Observatory spectra. Taking advantage of the low UV continuum and broad emission-line fluxes, we have determined that the deepest UV absorption component covers at least a portion of the inner, high-ionization narrow-line region (NLR). We find nonunity covering factors in the cores of several kinematic components, which increase the column density measurements of N V and C IV by factors of 1.2 to 1.9 over the full-covering case; however, the revised columns have only a minor effect on the parameters derived from our photoionization models. For the first time, we have simultaneous N V and C IV columns for component 1 (at -1040 km/s), and find that this component cannot be an X-ray warm absorber, contrary to our previous claim based on nonsimultaneous observations. We find that models of the absorbers based on solar abundances severely overpredict the O VI columns previously obtained with the Far Ultraviolet Spectrograph, and present arguments that this is not likely due to variability. However, models that include either enhanced nitrogen (twice solar) or dust, with strong depletion of carbon in either case, are successful in matching all of the observed ionic columns. These models result in substantially lower ionization parameters and total column densities compared to dust-free solar-abundance models, and produce little O VII or O VIII, indicating that none of the UV absorbers are X-ray warm absorbers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0305154v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0305154v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 May, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 5 figures (Figures 3 and 4 are in color), Accepted for publication in the Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 594 (2003) 116-127 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0208478">arXiv:astro-ph/0208478</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0208478">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0208478">ps</a>, <a href="https://arxiv.org/format/astro-ph/0208478">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/344542">10.1086/344542 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Kinematics and Physical Conditions pf the Ionized Gas in Markarian 509. II. STIS Echelle Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Crenshaw%2C+D+M">D. M. Crenshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Yaqoob%2C+T">T. Yaqoob</a>, <a href="/search/astro-ph?searchtype=author&query=McKernan%2C+B">B. McKernan</a>, <a href="/search/astro-ph?searchtype=author&query=Gabel%2C+J+R">J. R. Gabel</a>, <a href="/search/astro-ph?searchtype=author&query=George%2C+I+M">I. M. George</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+T+J">T. J. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">J. P. Dunn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0208478v1-abstract-short" style="display: inline;"> We present observations of the UV absorption lines in the luminous Seyfert 1 galaxy Mrk 509, obtained with the medium resolution (lambda/Delta-lambda ~ 40,000) echelle gratings of the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. The spectra reveal the presence of eight kinematic components of absorption in Ly-alpha, C IV, and N V, at radial velocities of -422, -328, -259,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0208478v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0208478v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0208478v1-abstract-full" style="display: none;"> We present observations of the UV absorption lines in the luminous Seyfert 1 galaxy Mrk 509, obtained with the medium resolution (lambda/Delta-lambda ~ 40,000) echelle gratings of the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. The spectra reveal the presence of eight kinematic components of absorption in Ly-alpha, C IV, and N V, at radial velocities of -422, -328, -259, -62, -22, +34, +124, and +210 km s^-1 with respect to an emission-line redshift of z = 0.03440, seven of which were detected in an earlier Far Ultraviolet Spectrographic Explorer (FUSE) spectrum. The component at -22 km s^-1 also shows absorption by Si IV. The covering factor and velocity width of the Si IV lines were lower than those of the higher ionization lines for this component, which is evidence for two separate absorbers at this velocity. We have calculated photoionization models to match the UV column densities in each of these components. Using the predicted O VI column densities, we were able to match the O VI profiles observed in the FUSE spectrum. Based on our results, none of the UV absorbers can produce the X-ray absorption seen in simultaneous Chandra observations; therefore, there must be more highly ionized gas in the radial velocity ranges covered by the UV absorbers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0208478v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0208478v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 August, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, three figures (Figure 1 is in color). Accepted for publication in the Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 582 (2003) 125-132 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 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