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156 results on '"Dalla Bonta, E."'

1. The Cepheid Distance to the Narrow-line Seyfert 1 Galaxy NGC 4051

Author

Yuan, W., Macri, L. M., Peterson, B. M., Riess, A. G., Fausnaugh, M. M., Hoffmann, S. L., Anand, G. S., Bentz, M. C., Dalla Bonta, E., Davies, R. I., De Rosa, G., Ferrarese, L., Grier, C. J., Hicks, E. K. S., Onken, C. A., Pogge, R. W., Storchi-Bergmann, T., Vestergaard, M., Yuan, W., Macri, L. M., Peterson, B. M., Riess, A. G., Fausnaugh, M. M., Hoffmann, S. L., Anand, G. S., Bentz, M. C., Dalla Bonta, E., Davies, R. I., De Rosa, G., Ferrarese, L., Grier, C. J., Hicks, E. K. S., Onken, C. A., Pogge, R. W., Storchi-Bergmann, T., and Vestergaard, M.

Abstract

We derive a distance of D = 16.6 +/- 0.3 Mpc (mu = 31.10 +/- 0.04 mag) to the archetypal narrow-line Seyfert 1 galaxy NGC 4051 based on Cepheid period-luminosity relations and new Hubble Space Telescope multiband imaging. We identify 419 Cepheid candidates and estimate the distance at both optical and near-infrared wavelengths using subsamples of precisely photometered variables (123 and 47 in the optical and near-infrared subsamples, respectively). We compare our independent photometric procedures and distance-estimation methods to those used by the Supernovae, H0, for the Equation of State team and find agreement to 0.01 mag. The distance we obtain suggests an Eddington ratio of m. approximate to 0.2 for NGC 4051, typical of narrow-line Seyfert 1 galaxies, unlike the seemingly odd value implied by previous distance estimates. We derive a peculiar velocity of -490 +/- 34 km s(-1) for NGC 4051, consistent with the overall motion of the Ursa Major Cluster in which it resides. We also revisit the energetics of the NGC 4051 nucleus, including its outflow and mass accretion rates.

Published
2021

2. Space Telescope and Optical Reverberation Mapping Project. XII. Broad-line Region Modeling of NGC 5548

Author

Williams, P. R., Pancoast, A., Treu, T., Brewer, B. J., Peterson, B. M., Barth, A. J., Malkan, M. A., De Rosa, G., Horne, Keith, Kriss, G. A., Arav, N., Bentz, M. C., Cackett, E. M., Dalla Bonta, E., Dehghanian, M., Done, C., Ferland, G. J., Grier, C. J., Kaastra, J., Kara, E., Kochanek, C. S., Mathur, S., Mehdipour, M., Pogge, R. W., Proga, D., Vestergaard, M., Waters, T., Adams, S. M., Anderson, M. D., Arevalo, P., Beatty, T. G., Bennert, V. N., Bigley, A., Bisogni, S., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Brotherton, M., Brown, J. E., Brown, J. S., Canalizo, G., Carini, M. T., Clubb, K. I., Comerford, J. M., Corsini, E. M., Crenshaw, D. M., Croft, S., Croxall, K. V., Deason, A. J., De Lorenzo-Caceres, A., Denney, K. D., Dietrich, M., Edelson, R., Efimova, N. V., Ely, J., Evans, P. A., Fausnaugh, M. M., Filippenko, A. V., Flatland, K., Fox, O. D., Gardner, E., Gates, E. L., Gehrels, N., Geier, S., Gelbord, J. M., Gonzalez, L., Gorjian, V., Greene, J. E., Grupe, D., Gupta, A., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W. -S., Hutchison, T., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Jones, J., Kaspi, S., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S., Kim, S. C., King, A., Klimanov, S. A., Knigge, C., Krongold, Y., Lau, M. W., Lee, J. C., Leonard, D. C., Li, Miao, Lira, P., Lochhaas, C., Ma, Zhiyuan, MacInnis, F., Manne-Nicholas, E. R., Mauerhan, J. C., McGurk, R., McHardy, I. M., Montuori, C., Morelli, L., Mosquera, A., Mudd, D., Muller-Sanchez, F., Nazarov, S. V., Norris, R. P., Nousek, J. A., Nguyen, M. L., Ochner, P., Okhmat, D. N., Papadakis, I., Parks, J. R., Pei, L., Penny, M. T., Pizzella, A., Poleski, R., Pott, J. -U., Rafter, S. E., Rix, H. -W., Runnoe, J., Saylor, D. A., Schimoia, J. S., Scott, B., Sergeev, S. G., Shappee, B. J., Shivvers, I., Siegel, M., Simonian, G. V., Siviero, A., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Sung, H. -I., Tayar, J., Tejos, N., Turner, C. S., Uttley, P., Van Saders, J., Vaughan, S. A., Vican, L., Villanueva, S., Villforth, C., Weiss, Y., Woo, J. -H., Yan, H., Young, S., Yuk, H., Zheng, W., Zhu, W., Zu, Y., Williams, P. R., Pancoast, A., Treu, T., Brewer, B. J., Peterson, B. M., Barth, A. J., Malkan, M. A., De Rosa, G., Horne, Keith, Kriss, G. A., Arav, N., Bentz, M. C., Cackett, E. M., Dalla Bonta, E., Dehghanian, M., Done, C., Ferland, G. J., Grier, C. J., Kaastra, J., Kara, E., Kochanek, C. S., Mathur, S., Mehdipour, M., Pogge, R. W., Proga, D., Vestergaard, M., Waters, T., Adams, S. M., Anderson, M. D., Arevalo, P., Beatty, T. G., Bennert, V. N., Bigley, A., Bisogni, S., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Brotherton, M., Brown, J. E., Brown, J. S., Canalizo, G., Carini, M. T., Clubb, K. I., Comerford, J. M., Corsini, E. M., Crenshaw, D. M., Croft, S., Croxall, K. V., Deason, A. J., De Lorenzo-Caceres, A., Denney, K. D., Dietrich, M., Edelson, R., Efimova, N. V., Ely, J., Evans, P. A., Fausnaugh, M. M., Filippenko, A. V., Flatland, K., Fox, O. D., Gardner, E., Gates, E. L., Gehrels, N., Geier, S., Gelbord, J. M., Gonzalez, L., Gorjian, V., Greene, J. E., Grupe, D., Gupta, A., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W. -S., Hutchison, T., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Jones, J., Kaspi, S., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S., Kim, S. C., King, A., Klimanov, S. A., Knigge, C., Krongold, Y., Lau, M. W., Lee, J. C., Leonard, D. C., Li, Miao, Lira, P., Lochhaas, C., Ma, Zhiyuan, MacInnis, F., Manne-Nicholas, E. R., Mauerhan, J. C., McGurk, R., McHardy, I. M., Montuori, C., Morelli, L., Mosquera, A., Mudd, D., Muller-Sanchez, F., Nazarov, S. V., Norris, R. P., Nousek, J. A., Nguyen, M. L., Ochner, P., Okhmat, D. N., Papadakis, I., Parks, J. R., Pei, L., Penny, M. T., Pizzella, A., Poleski, R., Pott, J. -U., Rafter, S. E., Rix, H. -W., Runnoe, J., Saylor, D. A., Schimoia, J. S., Scott, B., Sergeev, S. G., Shappee, B. J., Shivvers, I., Siegel, M., Simonian, G. V., Siviero, A., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Sung, H. -I., Tayar, J., Tejos, N., Turner, C. S., Uttley, P., Van Saders, J., Vaughan, S. A., Vican, L., Villanueva, S., Villforth, C., Weiss, Y., Woo, J. -H., Yan, H., Young, S., Yuk, H., Zheng, W., Zhu, W., and Zu, Y.

Abstract

We present geometric and dynamical modeling of the broad line region (BLR) for the multi-wavelength reverberation mapping campaign focused on NGC 5548 in 2014. The data set includes photometric and spectroscopic monitoring in the optical and ultraviolet, covering the H beta, Civ, and Ly alpha broad emission lines. We find an extended disk-like H beta BLR with a mixture of near-circular and outflowing gas trajectories, while the Civand Ly alpha BLRs are much less extended and resemble shell-like structures. There is clear radial structure in the BLR, with Civand Ly alpha emission arising at smaller radii than the H beta emission. Using the three lines, we make three independent black hole mass measurements, all of which are consistent. Combining these results gives a joint inference of log(10) (M-BH/M-circle dot) = 7.64(-0.18)(+0.21). We examine the effect of using the V band instead of the UV continuum light curve on the results and find a size difference that is consistent with the measured UV-optical time lag, but the other structural and kinematic parameters remain unchanged, suggesting that theVband is a suitable proxy for the ionizing continuum when exploring the BLR structure and kinematics. Finally, we compare the H beta results to similar models of data obtained in 2008 when the active galactic nucleus was at a lower luminosity state. We find that the size of the emitting region increased during this time period, but the geometry and black hole mass remained unchanged, which confirms that the BLR kinematics suitably gauge the gravitational field of the central black hole.

Published
2020

3. Intensive disc-reverberation mapping of Fairall 9:first year of Swift and LCO monitoring

Author

Santisteban, J. V. Hernandez, Edelson, R., Horne, K., Gelbord, J. M., Barth, A. J., Cackett, E. M., Goad, M. R., Netzer, H., Starkey, D., Uttley, P., Brandt, W. N., Korista, K., Lohfink, A. M., Onken, C. A., Page, K. L., Siegel, M., Vestergaard, M., Bisogni, S., Breeveld, A. A., Cenko, S. B., Dalla Bonta, E., Evans, P. A., Ferland, G., Gonzalez-Buitrago, D. H., Grupe, D., Joner, M. D., Kriss, G., LaPorte, S. J., Mathur, S., Marshall, F., Mehdipour, M., Mudd, D., Peterson, B. M., Schmidt, T., Vaughan, S., Valenti, S., Santisteban, J. V. Hernandez, Edelson, R., Horne, K., Gelbord, J. M., Barth, A. J., Cackett, E. M., Goad, M. R., Netzer, H., Starkey, D., Uttley, P., Brandt, W. N., Korista, K., Lohfink, A. M., Onken, C. A., Page, K. L., Siegel, M., Vestergaard, M., Bisogni, S., Breeveld, A. A., Cenko, S. B., Dalla Bonta, E., Evans, P. A., Ferland, G., Gonzalez-Buitrago, D. H., Grupe, D., Joner, M. D., Kriss, G., LaPorte, S. J., Mathur, S., Marshall, F., Mehdipour, M., Mudd, D., Peterson, B. M., Schmidt, T., Vaughan, S., and Valenti, S.

Abstract

We present results of time-series analysis of the first year of the Fairall 9 intensive disc-reverberation campaign. We used Swift and the Las Cumbres Observatory global telescope network to continuously monitor Fairall 9 from X-rays to near-infrared at a daily to subdaily cadence. The cross-correlation function between bands provides evidence for a lag spectrum consistent with the tau proportional to lambda(4/3) scaling expected for an optically thick, geometrically thin blackbody accretion disc. Decomposing the flux into constant and variable components, the variable component's spectral energy distribution is slightly steeper than the standard accretion disc prediction. We find evidence at the Balmer edge in both the lag and flux spectra for an additional bound-free continuum contribution that may arise from reprocessing in the broad-line region. The inferred driving light curve suggests two distinct components, a rapidly variable (100 d) component with an opposite lag to the reverberation signal.

Published
2020

4. The Cepheid Distance to the Seyfert 1 Galaxy NGC 4151

Author

Yuan, W., Fausnaugh, M. M., Hoffmann, S. L., Macri, L. M., Peterson, B. M., Riess, A. G., Bentz, M. C., Brown, J. S., Dalla Bonta, E., Davies, R., De Rosa, G., Ferrarese, L., Grier, C. J., Hicks, E. K. S., Onken, C. A., Pogge, R. W., Storchi-Bergmann, T., Vestergaard, M., Yuan, W., Fausnaugh, M. M., Hoffmann, S. L., Macri, L. M., Peterson, B. M., Riess, A. G., Bentz, M. C., Brown, J. S., Dalla Bonta, E., Davies, R., De Rosa, G., Ferrarese, L., Grier, C. J., Hicks, E. K. S., Onken, C. A., Pogge, R. W., Storchi-Bergmann, T., and Vestergaard, M.

Abstract

We derive a distance of 15.8 0.4 Mpc to the archetypal Seyfert 1 galaxy NGC 4151 based on the near-infrared Cepheid period-luminosity relation and new Hubble Space Telescope multiband imaging. This distance determination, based on measurements of 35 long-period (P> 25 days) Cepheids, will support the absolute calibration of the supermassive black hole mass in this system, as well as studies of the dynamics of the feedback or feeding of its active galactic nucleus.

Published
2020

5. Space Telescope and Optical Reverberation Mapping Project. XI. Disk-wind Characteristics and Contributions to the Very Broad Emission Lines of NGC 5548

Author

Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Korista, K. T., Goad, M. R., Chatzikos, M., Guzman, F., de Rosa, G., Mehdipour, M., Kaastra, J., Mathur, S., Vestergaard, M., Proga, D., Waters, T., Bentz, M. C., Bisogni, S., Brandt, W. N., Dalla Bonta, E., Fausnaugh, M. M., Gelbord, J. M., Horne, Keith, McHardy, I. M., Pogge, R. W., Starkey, D. A., Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Korista, K. T., Goad, M. R., Chatzikos, M., Guzman, F., de Rosa, G., Mehdipour, M., Kaastra, J., Mathur, S., Vestergaard, M., Proga, D., Waters, T., Bentz, M. C., Bisogni, S., Brandt, W. N., Dalla Bonta, E., Fausnaugh, M. M., Gelbord, J. M., Horne, Keith, McHardy, I. M., Pogge, R. W., and Starkey, D. A.

Abstract

In 2014 the NGC 5548 Space Telescope and Optical Reverberation Mapping campaign discovered a two-month anomaly when variations in the absorption and emission lines decorrelated from continuum variations. During this time the soft X-ray part of the intrinsic spectrum had been strongly absorbed by a line-of-sight (LOS) obscurer, which was interpreted as the upper part of a disk wind. Our first paper showed that changes in the LOS obscurer produces the decorrelation between the absorption lines and the continuum. A second study showed that the base of the wind shields the broad emission-line region (BLR), leading to the emission-line decorrelation. In that study, we proposed the wind is normally transparent with no effect on the spectrum. Changes in the wind properties alter its shielding and affect the spectral energy distribution (SED) striking the BLR, producing the observed decorrelations. In this work we investigate the impact of a translucent wind on the emission lines. We simulate the obscuration using XMM-Newton, NuSTAR, and Hubble Space Telescope observations to determine the physical characteristics of the wind. We find that a translucent wind can contribute a part of the Heiiand Fe K alpha emission. It has a modest optical depth to electron scattering, which explains the fainter far-side emission in the observed velocity-delay maps. The wind produces the very broad base seen in the UV emission lines and may also be present in the Fe K alpha line. Our results highlight the importance of accounting for the effects of such winds in the analysis of the physics of the central engine.

Published
2020

6. Space Telescope and Optical Reverberation Mapping Project. VI. Reverberating Disk Models for NGS 5548

Author

Starkey, D, Gehrels, Cornelis, Horne, Keith, Fausnaugh, M. M, Peterson, B. M, Bentz, M. C, Kochanek, C. S, Denney, K. D, Edelson, R, Goad, M. R, De Rosa, G, Anderson, M. D, Arevalo, P, Barth, A. J, Bazhaw, C, Borman, G. A, Boroson, T. A, Bottorff, M. C, Brandt, W. N, Breeveld, A. A, Cackett E. M, Carini, M. T, Croxall, K. V, Crenshaw, D. M, Dalla Bonta, E, De Lorenzo-Caceres, A, Dietrich, M, Efimova, N. V, Ely, J, Evans, P. A, Filippenko, A. V, Flatland, I, Gehrels, N, Geier, S, Gelbord, J. M, Gonzalez, L, Gorjian, V, Grier, C. J, Grupe, D, Hall, P. B, Hicks, S, Horenstein, D, Hutchison, T, Im, M, Jensen, J. J, Joner, M. D, Jones, J, Kaastra, J, Kaspi, S, Kelly, B. C, Kennea, J. A, Kim, S. C, Kim, M, Kilmanov, S. A, Korista, K. T, Kriss, G. A, Lee, J. C, Leonard, D. C, Lira, P, MacInnis, F, Manne-Nicholas, E. R, Mathur, S, McHardy, I. M, Montouri, C, Musso, R, Nazarov, S. V, Norris, R. P, Nousek, J. A, Okhmat, D. N, Pancoast, A, Parks, J. R, Pei, L, Pogge, R. W, Pott, J.-U, Rafter, S. E, Rix, H.-W, Saylor, D. A, Schimoia, J. S, Schnuelle, K, Sergeev, S. G, Siegel, M. H, Spencer, M, Sung, H. I, Teems, K. G, Turner, C. S, Uttley, P, Vestergaard, M, Villforth, C, Weiss, Y, Woo, J.-H, Yan, H, Young, S, Zheng, W, and Zu, Y

Subjects
Astrophysics
Abstract

We conduct a multi-wavelength continuum variability study of the Seyfert 1 galaxy NGC 5548 to investigate the temperature structure of its accretion disk. The 19 overlapping continuum light curves (1158 Angstrom to 9157 Angstrom) combine simultaneous Hubble Space Telescope, Swift, and ground-based observations over a 180 day period from 2014 January to July. Light-curve variability is interpreted as the reverberation response of the accretion disk to irradiation by a central time-varying point source. Our model yields the disk inclination i = 36deg +/- 10deg, temperature T(sub 1) = (44+/-6) times 10 (exp 3)K at 1 light day from the black hole, and a temperature radius slope (T proportional to r (exp -alpha)) of alpha = 0.99 +/- 0.03. We also infer the driving light curve and find that it correlates poorly with both the hard and soft X-ray light curves, suggesting that the X-rays alone may not drive the ultraviolet and optical variability over the observing period. We also decompose the light curves into bright, faint, and mean accretion-disk spectra. These spectra lie below that expected for a standard blackbody accretion disk accreting at L/L(sub Edd) = 0.1.

Published
2017
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7. Space Telescope and Optical Reverberation Mapping Project. VIII. Time Variability of Emission and Absorption in NGC 5548 Based on Modeling the Ultraviolet Spectrum

Author

Kriss, G. A., De Rosa, G., Ely, J., Peterson, B. M., Kaastra, J., Mehdipour, M., Ferland, G. J., Dehghanian, M., Mathur, S., Edelson, R., Arav, N., Barth, A. J., Bentz, M. C., Brandt, W. N., Crenshaw, D. M., Dalla Bonta, E., Denney, K. D., Done, C., Vestergaard, M., Adams, S. M., Anderson, M. D., Cackett, E. M., Canalizo, G., Cappi, M., Carini, M. T., Clubb, K., I, Comerford, J. M., Coker, C. T., Corsini, E. M., Costantini, E., Croft, S., Croxall, K., V, Deason, A. J., Gorjian, V, Grupe, D., Gupta, A., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W-S, Hutchison, T. A., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Kaspi, S., Kelly, B. C., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S. C., Kim, S. Y., King, A., Klimanov, S. A., Krongold, Y., Runnoe, J., Saylor, D. A., Schimoia, J. S., Schnuelle, K., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Villanueva, S., Jr., Walton, D. J., Kriss, G. A., De Rosa, G., Ely, J., Peterson, B. M., Kaastra, J., Mehdipour, M., Ferland, G. J., Dehghanian, M., Mathur, S., Edelson, R., Arav, N., Barth, A. J., Bentz, M. C., Brandt, W. N., Crenshaw, D. M., Dalla Bonta, E., Denney, K. D., Done, C., Vestergaard, M., Adams, S. M., Anderson, M. D., Cackett, E. M., Canalizo, G., Cappi, M., Carini, M. T., Clubb, K., I, Comerford, J. M., Coker, C. T., Corsini, E. M., Costantini, E., Croft, S., Croxall, K., V, Deason, A. J., Gorjian, V, Grupe, D., Gupta, A., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W-S, Hutchison, T. A., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Kaspi, S., Kelly, B. C., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S. C., Kim, S. Y., King, A., Klimanov, S. A., Krongold, Y., Runnoe, J., Saylor, D. A., Schimoia, J. S., Schnuelle, K., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Villanueva, S., Jr., and Walton, D. J.

Abstract

We model the ultraviolet spectra of the Seyfert 1 galaxy NGC 5548 obtained with the Hubble Space Telescope during the 6 month reverberation mapping campaign in 2014. Our model of the emission from NGC 5548 corrects for overlying absorption and deblends the individual emission lines. Using the modeled spectra, we measure the response to continuum variations for the deblended and absorption-corrected individual broad emission lines, the velocity-dependent profiles of Ly and C iv, and the narrow and broad intrinsic absorption features. We find that the time lags for the corrected emission lines are comparable to those for the original data. The velocity-binned lag profiles of Ly and C iv have a double-peaked structure indicative of a truncated Keplerian disk. The narrow absorption lines show a delayed response to continuum variations corresponding to recombination in gas with a density of ∼105 cm-3. The high-ionization narrow absorption lines decorrelate from continuum variations during the same period as the broad emission lines. Analyzing the response of these absorption lines during this period shows that the ionizing flux is diminished in strength relative to the far-ultraviolet continuum. The broad absorption lines associated with the X-ray obscurer decrease in strength during this same time interval. The appearance of X-ray obscuration in ∼2012 corresponds with an increase in the luminosity of NGC 5548 following an extended low state. We suggest that the obscurer is a disk wind triggered by the brightening of NGC 5548 following the decrease in size of the broad-line region during the preceding low-luminosity state.

Published
2019

8. A slow bar in the lenticular barred galaxy NGC 4277

Author

Buttitta, C, Corsini, E M, Cuomo, V, Aguerri, J A L, Coccato, L, Costantin, L, Dalla Bonta, E, Debattista, Victor P, Iodice, E, Méndez-Abreu, J, Morelli, L, and Pizzella, A

Subjects
galaxies: photometry, F520, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), F521, galaxies: structure, FOS: Physical sciences, Astronomy and Astrophysics, galaxies: evolution, galaxies: individual: NGC4277, galaxies: kinematics and dynamics, Astrophysics - Astrophysics of Galaxies
Abstract

Aims: We characterised the properties of the bar hosted in lenticular galaxy NGC 4277, which is located behind the Virgo cluster. Methods: We measured the bar length and strength from the surface photometry obtained from the broad-band imaging of the Sloan Digital Sky Survey and we derived the bar pattern speed from the stellar kinematics obtained from the integral-field spectroscopy performed with the Multi Unit Spectroscopic Explorer at the Very Large Telescope. We also estimated the co-rotation radius from the circular velocity, which we constrained by correcting the stellar streaming motions for asymmetric drift, and we finally derived the bar rotation rate. Results: We found that NGC 4277 hosts a short ($R_{bar}=3.2^{+0.9}_{-0.6}$ kpc), weak ($S_{bar}=0.21 \pm 0.02$), and slow ($R=1.8^{+0.5}_ {-0.3}$) bar and its pattern speed ($\Omega_{bar}=24.7\pm3.4$ km s$^{-1}$ kpc$^{-1}$) is amongst the best-constrained ones ever obtained with the Tremaine-Weinberg (TW) method with relative statistical errors of $\sim0.2$. Conclusions: NGC 4277 is the first clear-cut case of a galaxy hosting a slow stellar bar ($R>1.4$ at more than a 1$\sigma$ confidence level) measured with the model-independent TW method. A possible interaction with the neighbour galaxy NGC 4273 could have triggered the formation of such a slow bar and/or the bar could be slowed down due to the dynamical friction with a significant amount of dark matter within the bar region., Comment: Accepted for publication on A&A, 10 pages

Published
2022

9. Velocity-resolved Reverberation Mapping of Five Bright Seyfert 1 Galaxies

Author

De Rosa, G., Fausnaugh, M. M., Grier, C. J., Peterson, B. M., Denney, K. D., Horne, Keith, Ciroi, S., Dalla Bonta, E., Joner, M. D., Kaspi, S., Kochanek, C. S., Pogge, R. W., Sergeev, S. G., Vestergaard, M., Adams, S. M., Antognini, J., Salvo, C. Araya, Armstrong, E., Bae, J., Barth, A. J., Beatty, T. G., Bhattacharjee, A., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brown, J. E., Brown, J. S., Brotherton, M. S., Coker, C. T., Clanton, C., Cracco, V., Crawford, S. M., Croxall, K. V., Eftekharzadeh, S., Eracleous, M., Fiorenza, S. L., Frassati, A., Hawkins, K., Henderson, C. B., Holoien, T. W. -S., Hutchison, T., Kellar, J., Kilerci-Eser, E., Kim, S., King, A. L., La Mura, G., Laney, C. D., Lochhaas, C., Ma, Z., MacInnis, F., De Rosa, G., Fausnaugh, M. M., Grier, C. J., Peterson, B. M., Denney, K. D., Horne, Keith, Ciroi, S., Dalla Bonta, E., Joner, M. D., Kaspi, S., Kochanek, C. S., Pogge, R. W., Sergeev, S. G., Vestergaard, M., Adams, S. M., Antognini, J., Salvo, C. Araya, Armstrong, E., Bae, J., Barth, A. J., Beatty, T. G., Bhattacharjee, A., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brown, J. E., Brown, J. S., Brotherton, M. S., Coker, C. T., Clanton, C., Cracco, V., Crawford, S. M., Croxall, K. V., Eftekharzadeh, S., Eracleous, M., Fiorenza, S. L., Frassati, A., Hawkins, K., Henderson, C. B., Holoien, T. W. -S., Hutchison, T., Kellar, J., Kilerci-Eser, E., Kim, S., King, A. L., La Mura, G., Laney, C. D., Lochhaas, C., Ma, Z., and MacInnis, F.

Published
2018

10. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. VI. REVERBERATING DISK MODELS FOR NGC 5548

Author

Starkey, D., Horne, Keith, Fausnaugh, M. M., Peterson, B. M., Bentz, M. C., Kochanek, C. S., Denney, K. D., Edelson, R., Goad, M. R., De Rosa, G., Anderson, M. D., Arevalo, P., Barth, A. J., Bazhaw, C., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Cackett, E. M., Carini, M. T., Croxall, K. V., Crenshaw, D. M., Dalla Bonta, E., De Lorenzo-Caceres, A., Dietrich, M., Efimova, N. V., Ely, J., Evans, P. A., Filippenko, A. V., Flatland, K., Gehrels, N., Geier, S., Gelbord, J. M., Gonzalez, L., Gorjian, V., Grier, C. J., Grupe, D., Hall, P. B., Hicks, S., Horenstein, D., Hutchison, T., Im, M., Jensen, J. J., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kennea, J. A., Kim, S. C., Kim, M., Klimanov, S. A., Korista, K. T., Kriss, G. A., Lee, J. C., Leonard, D. C., Lira, P., MacInnis, F., Manne-Nicholas, E. R., Mathur, S., McHardy, I. M., Montouri, C., Musso, R., Nazarov, S. V., Norris, R. P., Nousek, J. A., Okhmat, D. N., Pancoast, A., Parks, J. R., Pei, L., Pogge, R. W., Pott, J-U, Rafter, S. E., Rix, H-W, Saylor, D. A., Schimoia, J. S., Schnuelle, K., Sergeev, S. G., Siegel, M. H., Spencer, M., Sung, H-I, Teems, K. G., Turner, C. S., Uttley, P., Vestergaard, M., Villforth, C., Weiss, Y., Woo, J-H, Yan, H., Young, S., Zheng, W., Zu, Y., Starkey, D., Horne, Keith, Fausnaugh, M. M., Peterson, B. M., Bentz, M. C., Kochanek, C. S., Denney, K. D., Edelson, R., Goad, M. R., De Rosa, G., Anderson, M. D., Arevalo, P., Barth, A. J., Bazhaw, C., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Cackett, E. M., Carini, M. T., Croxall, K. V., Crenshaw, D. M., Dalla Bonta, E., De Lorenzo-Caceres, A., Dietrich, M., Efimova, N. V., Ely, J., Evans, P. A., Filippenko, A. V., Flatland, K., Gehrels, N., Geier, S., Gelbord, J. M., Gonzalez, L., Gorjian, V., Grier, C. J., Grupe, D., Hall, P. B., Hicks, S., Horenstein, D., Hutchison, T., Im, M., Jensen, J. J., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kennea, J. A., Kim, S. C., Kim, M., Klimanov, S. A., Korista, K. T., Kriss, G. A., Lee, J. C., Leonard, D. C., Lira, P., MacInnis, F., Manne-Nicholas, E. R., Mathur, S., McHardy, I. M., Montouri, C., Musso, R., Nazarov, S. V., Norris, R. P., Nousek, J. A., Okhmat, D. N., Pancoast, A., Parks, J. R., Pei, L., Pogge, R. W., Pott, J-U, Rafter, S. E., Rix, H-W, Saylor, D. A., Schimoia, J. S., Schnuelle, K., Sergeev, S. G., Siegel, M. H., Spencer, M., Sung, H-I, Teems, K. G., Turner, C. S., Uttley, P., Vestergaard, M., Villforth, C., Weiss, Y., Woo, J-H, Yan, H., Young, S., Zheng, W., and Zu, Y.

Published
2017

11. Space Telescope and Optical Reverberation Mapping Project. V. Optical Spectroscopic Campaign and Emission-line Analysis for NGC 5548

Author

Pei, L., Fausnaugh, M. M., Barth, A. J., Peterson, B. M., Bentz, M. C., De Rosa, G., Denney, K. D., Goad, M. R., Kochanek, C. S., Korista, K. T., Pogge, R. W., Clubb, K. I., Dalla Bonta, E., Filippenko, A. V., Greene, J. E., Grier, C. J., Vestergaard, M., Zheng, W., Adams, Scott M., Beatty, Thomas G., Bigley, A., Brown, Jacob E., Brown, Jonathan S., Canalizo, G., Gates, E. L., Lochhaas, Cassandra, Ma, Zhiyuan, Manne-Nicholas, E. R., Mauerhan, J. C., Malkan, M. A., McGurk, R., Morelli, L., Mosquera, Ana, Mudd, Dale, Sanchez, F. Muller, Nguyen, M. L., Ochner, P., Ou-Yang, B., Pancoast, A., Penny, Matthew T., Pizzella, A., Poleski, Radoslaw, Runnoe, Jessie, Scott, B., Schimoia, Jaderson S., Cackett, E. M., Carini, M. T., Crenshaw, D. M., De Lorenzo-Caceres, A., Dietrich, M., Edelson, R., Efimova, N. V., Ely, J., Evans, P. A., Ferland, G. J., Flatland, K., Gehrels, N., Geier, S., Gelbord, J. M., Grupe, D., Gupta, A., Hall, P. B., Hicks, S., Horenstein, D., Im, M., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kennea, J. A., Papadakis, I., Parks, J. R., Rix, H. -W., Schnuelle, K., Sergeev, S. G., Siegel, M., Skielboe, A., Spencer, M., Starkey, D., Sung, H. -I., Teems, K. G., Villforth, C., Weiss, Y., Pei, L., Fausnaugh, M. M., Barth, A. J., Peterson, B. M., Bentz, M. C., De Rosa, G., Denney, K. D., Goad, M. R., Kochanek, C. S., Korista, K. T., Pogge, R. W., Clubb, K. I., Dalla Bonta, E., Filippenko, A. V., Greene, J. E., Grier, C. J., Vestergaard, M., Zheng, W., Adams, Scott M., Beatty, Thomas G., Bigley, A., Brown, Jacob E., Brown, Jonathan S., Canalizo, G., Gates, E. L., Lochhaas, Cassandra, Ma, Zhiyuan, Manne-Nicholas, E. R., Mauerhan, J. C., Malkan, M. A., McGurk, R., Morelli, L., Mosquera, Ana, Mudd, Dale, Sanchez, F. Muller, Nguyen, M. L., Ochner, P., Ou-Yang, B., Pancoast, A., Penny, Matthew T., Pizzella, A., Poleski, Radoslaw, Runnoe, Jessie, Scott, B., Schimoia, Jaderson S., Cackett, E. M., Carini, M. T., Crenshaw, D. M., De Lorenzo-Caceres, A., Dietrich, M., Edelson, R., Efimova, N. V., Ely, J., Evans, P. A., Ferland, G. J., Flatland, K., Gehrels, N., Geier, S., Gelbord, J. M., Grupe, D., Gupta, A., Hall, P. B., Hicks, S., Horenstein, D., Im, M., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kennea, J. A., Papadakis, I., Parks, J. R., Rix, H. -W., Schnuelle, K., Sergeev, S. G., Siegel, M., Skielboe, A., Spencer, M., Starkey, D., Sung, H. -I., Teems, K. G., Villforth, C., and Weiss, Y.

Published
2017

12. Space Telescope and Optical Reverberation Mapping Project. X. Understanding the Absorption-line Holiday in NGC 5548

Author

Physics, Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Mathur, S., Mehdipour, M., Guzman, F., Chatzikos, M., van Hoof, P. A. M., Williams, R. J. R., Arav, Nahum, Barth, A. J., Bentz, M. C., Bisogni, S., Brandt, W. N., Crenshaw, D. M., Dalla Bonta, E., De Rosa, G., Fausnaugh, M. M., Gelbord, J. M., Goad, M. R., Gupta, A., Horne, Keith, Kaastra, J., Knigge, C., Korista, K. T., McHardy, I. M., Pogge, R. W., Starkey, D. A., Vestergaard, M., Physics, Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Mathur, S., Mehdipour, M., Guzman, F., Chatzikos, M., van Hoof, P. A. M., Williams, R. J. R., Arav, Nahum, Barth, A. J., Bentz, M. C., Bisogni, S., Brandt, W. N., Crenshaw, D. M., Dalla Bonta, E., De Rosa, G., Fausnaugh, M. M., Gelbord, J. M., Goad, M. R., Gupta, A., Horne, Keith, Kaastra, J., Knigge, C., Korista, K. T., McHardy, I. M., Pogge, R. W., Starkey, D. A., and Vestergaard, M.

Abstract

The Space Telescope and Optical Reverberation Mapping Project (AGN STORM) on NGC 5548 in 2014 is one of the most intensive multiwavelength AGN monitoring campaigns ever. For most of the campaign, the emission-line variations followed changes in the continuum with a time lag, as expected. However, the lines varied independently of the observed UV-optical continuum during a 60-70 day "holiday," suggesting that unobserved changes to the ionizing continuum were present. To understand this remarkable phenomenon and to obtain an independent assessment of the ionizing continuum variations, we study the intrinsic absorption lines present in NGC 5548. We identify a novel cycle that reproduces the absorption line variability and thus identify the physics that allows the holiday to occur. In this cycle, variations in this obscurer's line-of-sight covering factor modify the soft X-ray continuum, changing the ionization of helium Ionizing radiation produced by recombining helium then affects the level of ionization of some ions seen by the Hubble Space Telescope. In particular, high-ionization species are affected by changes in the obscurer covering factor, which does not affect the optical or UV continuum, and thus appear as uncorrelated changes, a "holiday." It is likely that any other model that selectively changes the soft X-ray part of the continuum during the holiday can also explain the anomalous emission-line behavior observed.

Published
2019

13. Space Telescope and Optical Reverberation Mapping Project. IV. Anomalous Behavior of the Broad Ultraviolet Emission Lines in NGC 5548

Author

Goad, M. R., Korista, K. T., De Rosa, G., Kriss, G. A., Edelson, R., Barth, A. J., Ferland, G. J., Kochanek, C. S., Peterson, B. M., Denney, K. D., Pei, L., Skielboe, A., Starkey, D., Vestergaard, M., Zu, Y., Anderson, M. D., Arevalo, P., Borman, G. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Brewer, B. J., Cackett, E. M., Carini, M. T., Croxall, K. V., Dalla Bonta, E., De Lorenzo-Caceres, A., Efimova, N. V., Filippenko, A. V., Gelbord, J. M., Hutchison, T., Im, M., Jensen, J. J., Joner, M. D., Goad, M. R., Korista, K. T., De Rosa, G., Kriss, G. A., Edelson, R., Barth, A. J., Ferland, G. J., Kochanek, C. S., Peterson, B. M., Denney, K. D., Pei, L., Skielboe, A., Starkey, D., Vestergaard, M., Zu, Y., Anderson, M. D., Arevalo, P., Borman, G. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Brewer, B. J., Cackett, E. M., Carini, M. T., Croxall, K. V., Dalla Bonta, E., De Lorenzo-Caceres, A., Efimova, N. V., Filippenko, A. V., Gelbord, J. M., Hutchison, T., Im, M., Jensen, J. J., and Joner, M. D.

Published
2016

14. Data and two-dimensional scaling relations for galaxies in Abell 1689: a hint of size evolution at z similar to 0.2

Author

Houghton, RCW, Davies, RL, Dalla Bonta, E, and Masters, R

Abstract

We present imaging and spectroscopy of Abell 1689 (z= 0.183) from the Gemini multi-object spectrograph (GMOS) on the Gemini North telescope and the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope (HST). We measure integrated photometry from the GMOS g' and r' images (for 531 galaxies) and surface photometry from the HSTF625W image (for 43 galaxies) as well as velocities and velocity dispersions from the GMOS spectra (for 71 galaxies). We construct the Kormendy, Faber-Jackson and colour-magnitude relations for early-type galaxies in Abell 1689 using these data and compare them to those of the Coma cluster. We measure the intrinsic scatter of the colour-magnitude relation in Abell 1689 to be σ CMR= 0.054 ± 0.004mag, which places degenerate constraints on the ratio of the assembly time-scale to the time available (β) and the age of the population. Making the assumption that galaxies in Abell 1689 will evolve into those of Coma over an interval of 2.26Gyr breaks this degeneracy and limits β to be >0.6 and the age of the red sequence to be >5.5Gyr (formed at z > 0.55). Without corrections for size evolution but accounting for magnitude cuts and selection effects, the Kormendy and Faber-Jackson relations are inconsistent and disagree at the 2σ level regarding the amount of luminosity evolution in the last 2.26Gyr. However, after correcting for size evolution the Kormendy and Faber-Jackson relations show similar changes in luminosity (0.22 ± 0.11mag) that are consistent with the passive evolution of the stellar populations from a single burst of star formation 10.2 ± 3.3Gyr ago (). Thus, the changes in the Kormendy, Faber-Jackson and colour-magnitude relations of Abell 1689 relative to Coma all agree and suggest old galaxy populations with little or no synchronization in the star formation histories. Furthermore, the weak evidence for size evolution in the cluster environment in the last 2.26Gyr places interesting constraints on the possible mechanisms at work, favouring harassment or secular processes over merger scenarios. © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS.

Published
2016

18. Searching for nuclear stellar discs in simulations of star cluster mergers

Author

Portaluri, E., Corsini, E. M., Morelli, L., Hartmann, M., Dalla Bonta, E., Debattista, Victor P, Pizzella, A., Portaluri, E., Corsini, E. M., Morelli, L., Hartmann, M., Dalla Bonta, E., Debattista, Victor P, and Pizzella, A.

Abstract

The nuclei of galaxies often host small stellar discs with scalelengths of a few tens of parsecs and luminosities up to 107 L�. To investigate the formation and properties of nuclear stellar discs (NSDs), we look for their presence in a set of N-body simulations studying the dissipationless merging of multiple star clusters in galactic nuclei. A few tens of star clusters with sizes and masses comparable to those of globular clusters observed in the Milky Way are accreted on to a pre-existing nuclear stellar component: either a massive super star cluster or a rapidly rotating, compact disc with a scalelength of a few parsecs, mimicking the variety of observed nuclear structures. Images and kinematic maps of the simulation time-steps are then built and analysed as if they were real and at the distance of the Virgo cluster. We use the Scorza–Bender method to search for the presence of disc structures via photometric decomposition. In one case, the merger remnant has all the observed photometric and kinematic properties of NSDs observed in real galaxies. This shows that current observations are consistent with most of the NSD mass being assembled from the migration and accretion of star clusters into the galactic centre. In the other simulation instead, we detect an elongated structure from the unsharp masked image, that does not develop the photometric or kinematic signature of an NSD. Thus, in the context of searches for a disc structure, the Scorza–Bender method is a robust and necessary tool.

Published
2013

19. Fast and slow rotators in the densest environments: a FLAMES/GIRAFFE integral field spectroscopy study of galaxies in A1689 at z=0.183

Author

D'Eugenio, Francesco, Houghton, Ryan C W, Davies, Roger L, Dalla Bonta, E, D'Eugenio, Francesco, Houghton, Ryan C W, Davies, Roger L, and Dalla Bonta, E

Abstract

We present FLAMES/GIRAFFE integral field spectroscopy of 30 galaxies in the massive cluster A1689 at z = 0.183. Conducting an analysis similar to that of ATLAS3D, we extend the baseline of the kinematic morphology–density relation by an order of magnitude in projected density and show that it is possible to use existing instruments to identify slow and fast rotators beyond the local Universe. We find 4.5 ± 1.0 slow rotators with a distribution in magnitude similar to those in the Virgo cluster. The overall slow rotator fraction of our A1689 sample is 0.15 ± 0.03, the same as in Virgo using our selection criteria. This suggests that the fraction of slow rotators in a cluster is not strongly dependent on its density. However, within A1689, we find that the fraction of slow rotators increases towards the centre, as was also found in the Virgo cluster.

Published
2013

22. VizieR Online Data Catalog: Space telescope RM project. III. NGC 5548 LCs (Fausnaugh+, 2016)

Author

Fausnaugh, M. M., Denney, K. D., Barth, A. J., Bentz, M. C., Bottorff, M. C., Carini, M. T., Croxall, K. V., Rosa, G., Goad, M. R., Horne, K., Joner, M. D., Kaspi, S., Kim, M., Klimanov, S. A., Kochanek, C. S., Leonard, D. C., Netzer, H., Peterson, B. M., Schnulle, K., Sergeev, S. G., Marianne Vestergaard, Zheng, W., Zu, Y., Anderson, M. D., Arevalo, P., Bazhaw, C., Borman, G. A., Boroson, T. A., Brandt, W. N., Breeveld, A. A., Brewer, B. J., Cackett, E. M., Crenshaw, D. M., Dalla Bonta, E., Lorenzo-Caceres, A., Dietrich, M., Edelson, R., Efimova, N. V., Ely, J., Evans, P. A., Filippenko, A. V., Flatland, K., Gehrels, N., Geier, S., Gelbord, J. M., Gonzalez, L., Gorjian, V., Grier, C. J., Grupe, D., Hall, P. B., Hicks, S., Horenstein, D., Hutchison, T., Im, M., Jensen, J. J., Jones, J., Kaastra, J., Kelly, B. C., Kennea, J. A., Kim, S. C., Korista, K. T., Kriss, G. A., Lee, J. C., Lira, P., Macinnis, F., Manne-Nicholas, E. R., Mathur, S., Mchardy, I. M., Montouri, C., Musso, R., Nazarov, S. V., Norris, R. P., Nousek, J. A., Okhmat, D. N., Pancoast, A., Papadakis, I., Parks, J. R., Pei, L., Pogge, R. W., Pott, J. -U, Rafter, S. E., Rix, H., Saylor, D. A., Schimoia, J. S., Siegel, M., Spencer, M., Starkey, D., Sung, H., Teems, K. G., Treu, T., Turner, C. S., Uttley, P., Villforth, C., Weiss, Y., Woo, J., Yan, H., and Young, S.

23. VizieR Online Data Catalog

Author

Rosa, G., Peterson, B. M., Ely, J., Kriss, G. A., Crenshaw, D. M., Horne, K., Korista, K. T., Netzer, H., Pogge, R. W., Arevalo, P., Barth, A. J., Brandt, W. N., Breeveld, A. A., Brewer, B. J., Dalla Bonta, E., Lorenzo-Caceres, A., Denney, K. D., Dietrich, M., Edelson, R., Evans, P. A., Fausnaugh, M. M., Gehrels, N., Gelbord, J. M., Goad, M. R., Grier, C. J., Grupe, D., Hall, P. B., Kaastra, J., Kelly, B. C., Kennea, J. A., Kochanek, C. S., Lira, P., Mathur, S., Mchardy, I. M., Nousek, J. A., Pancoast, A., Papadakis, I., Pei, L., Schimoia, J. S., Siegel, M., Starkey, D., Treu, T., Uttley, P., Vaughan, S., Marianne Vestergaard, Villforth, C., Young, S., Zu, Y., and AGN STORM

24. Denaro falso

Author

Tolstoj Lev and Tolstoj Lev

Abstract

Denaro falso, racconto in due parti scritto non prima del 1904, fu pubblicato postumo nel 1911. Da subito venne considerato una requisitoria contro il denaro, inteso come strumento di corruzione individuale e sociale. In realtà è molto più di questo: è la continuazione ideale dell'ultimo grande romanzo di Tolstoj, Resurrezione, che si conclude con l'affermazione del potere di redenzione del Vangelo. Anche qui la forza della sacra scrittura viene sostenuta con decisione dall'autore, in contrapposizione al potere di corruzione del denaro. L'interminabile catena di eventi causati da un singolo peccato giovanile si intreccia con una ben più potente catena di eventi originati dalla bontà, e da questa viene distrutta e trasformata.

Published
2024

25. Black holes in close binary systems and galactic nuclei.

Author

Cherepashchuk, A.

Subjects
BLACK holes, BINARY systems (Astronomy), GALACTIC nuclei, X-ray binaries, GRAVITATIONAL waves
Abstract

After 50 years of observational studies of black holes, great progress has been achieved in this branch of astrophysics. Several dozen stellar-mass black holes have been discovered in X-ray binaries, and several hundred supermassive black holes in galactic nuclei. The remarkable recent discovery of gravitational waves from merging black holes in a binary system by LIGO marks the beginning of a new stage in black-hole research. It is quite possible that gravitational-wave studies will provide definitive evidence for the existence of event horizons in black holes in the near future. On the other hand, the development of methods for space and ground-based radio-interferometry observations provides hope that it will be possible to obtain images of 'shadows' of supermassive black holes in galactic nuclei, and to observe directly processes occurring in the vicinities of the event horizons of supermassive black holes. This is important for tests of general relativity in extremely strong gravitational fields. [ABSTRACT FROM AUTHOR]

Published
2017
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26. Intensive disc-reverberation mapping of Fairall 9

Author

S. Valenti, A. A. Breeveld, W. N. Brandt, J. M. Gelbord, D. A. Starkey, M. H. Siegel, Marianne Vestergaard, K. L. Page, Bradley M. Peterson, Dirk Grupe, Christopher A. Onken, Kirk T. Korista, S. J. Laporte, E. Dalla Bontà, D. Mudd, Smita Mathur, Phil Uttley, Aaron J. Barth, Michael D. Joner, P. A. Evans, Gerard A. Kriss, Hagai Netzer, D. Gonzalez-Buitrago, J. V. Hernández Santisteban, M. R. Goad, Gary J. Ferland, T. Schmidt, Susanna Bisogni, Anne M. Lohfink, Keith Horne, Rick Edelson, Edward M. Cackett, S. B. Cenko, Simon Vaughan, Missagh Mehdipour, F. E. Marshall, ITA, USA, GBR, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
ACTIVE GALACTIC NUCLEI, CONTINUUM EMISSION, Astrophysics::High Energy Astrophysical Phenomena, individual: Fairall 9 [quasars], BROAD-LINE REGION, SOFTWARE, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, law.invention, Telescope, symbols.namesake, VIEW, Observatory, law, 0103 physical sciences, DISTRIBUTIONS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, LAGS, Physics, 010308 nuclear & particles physics, Balmer series, Astronomy and Astrophysics, Quasar, Light curve, VARIABILITY, Space and Planetary Science, active [galaxies], X-RAY, symbols, Reverberation mapping, Spectral energy distribution, accretion, accretion discs, ACCRETION DISC
Abstract

We present results of time-series analysis of the first year of the Fairall 9 intensive disc-reverberation campaign. We used Swift and the Las Cumbres Observatory global telescope network to continuously monitor Fairall 9 from X-rays to near-infrared at a daily to subdaily cadence. The cross-correlation function between bands provides evidence for a lag spectrum consistent with the τ ∝ λ4/3 scaling expected for an optically thick, geometrically thin blackbody accretion disc. Decomposing the flux into constant and variable components, the variable component’s spectral energy distribution is slightly steeper than the standard accretion disc prediction. We find evidence at the Balmer edge in both the lag and flux spectra for an additional bound-free continuum contribution that may arise from reprocessing in the broad-line region. The inferred driving light curve suggests two distinct components, a rapidly variable (100 d) component with an opposite lag to the reverberation signal.

Published
2020

27. Space Telescope and Optical Reverberation Mapping Project. XII: Broad-line Region Modeling of NGC 5548

Author

Christopher S. Kochanek, T. Hutchison, H. W. Rix, Gary J. Ferland, Alessandro Pizzella, E. Holmbeck, E. R. Manne-Nicholas, Ori D. Fox, Radosław Poleski, I. E. Papadakis, Erin Kara, S. Young, Vardha N. Bennert, Kelly D. Denney, Daniel J. Stevens, M. Dietrich, Calen B. Henderson, WeiKang Zheng, Haojing Yan, Aaron J. Barth, P. Lira, M. C. Bottorff, Steve Croft, Jelle Kaastra, Jamie Tayar, Misty C. Bentz, Zhiyuan Ma, Laura Vican, Jenny E. Greene, J. S. Brown, M. W. Lau, F. Müller-Sánchez, Alexei V. Filippenko, Dirk Grupe, Daniel Proga, R. McGurk, Alis J. Deason, I. M. McHardy, K. Flatland, Matthew A. Malkan, Michael D. Joner, Douglas C. Leonard, Kelsey I. Clubb, Missagh Mehdipour, B. J. Shappee, Kevin V. Croxall, J. M. Gelbord, M. H. Siegel, Jon C. Mauerhan, Ying Zu, Patrick L. Kelly, Christian Knigge, Myungshin Im, Peter R. Williams, C. A. Johnson, S. V. Nazarov, J. A. Nousek, Miao Li, C. S. Turner, Andrew J. King, Marianne Vestergaard, S. C. Kim, G. De Rosa, J. R. Parks, M. Spencer, S. G. Sergeev, Steven Villanueva, Matthew T. Penny, Lorenzo Morelli, Jong-Hak Woo, D. Mudd, D. M. Crenshaw, J.-U. Pott, T. W. S. Holoien, A. A. Breeveld, D. N. Okhmat, Scott M. Adams, Carolin Villforth, Sang Chul Kim, V. Gorjian, W. N. Brandt, G. V. Simonian, Elinor L. Gates, Shai Kaspi, M. Dehghanian, D. A. Saylor, Hyun-Il Sung, Simon Vaughan, Isaac Shivvers, F. MacInnis, Minjin Kim, Edward M. Cackett, Liuyi Pei, Alessandro Siviero, Cassandra Lochhaas, Patrick B. Hall, Wei Zhu, Tommaso Treu, Thomas G. Beatty, Tim Waters, B. Scott, J. C. Lee, Jeremy Jones, M. L. Nguyen, Ryan Norris, Susanna Bisogni, Justin Ely, Keith Horne, A. Gupta, L. Gonzalez, J. J. Jensen, P. Arévalo, N. Gehrels, Catherine J. Grier, S. Geier, Enrico Maria Corsini, S. E. Rafter, P. Ochner, Y. Weiss, A. Skielboe, Michael T. Carini, Michael S. Brotherton, H. Yuk, Chris Done, Gerard A. Kriss, C. Montuori, Bradley M. Peterson, E. Dalla Bontà, Emma Gardner, D. A. Starkey, R. W. Pogge, Smita Mathur, J. A. Kennea, P. A. Evans, A. Bigley, Jessie C. Runnoe, S. Hicks, S. A. Klimanov, Todd Boroson, J. van Saders, J. S. Schimoia, Garrett Somers, Phil Uttley, Nahum Arav, G. A. Borman, J. E. Brown, Nicolas Tejos, Julia M. Comerford, A. de Lorenzo-Cáceres, Gabriela Canalizo, Ana M. Mosquera, A. Pancoast, Michael Fausnaugh, Rick Edelson, N. V. Efimova, Brendon J. Brewer, Yair Krongold, High Energy Astrophys. & Astropart. Phys (API, FNWI), University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, ITA, USA, and GBR

Subjects
010504 meteorology & atmospheric sciences, Active galaxies, Active galactic nuclei, Reverberation mapping, Seyfert galaxies, Astrophysics, 01 natural sciences, Atomic, Particle and Plasma Physics, Reverberation mapping, Spitzer Space Telescope, Emission spectrum, 010303 astronomy & astrophysics, QC, Physics, Seyfert galaxies, Balmer series, 3rd-DAS, VARIABILITY, Reverbation mapping, AGN MONITORING PROJECT, symbols, STEPS, Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Active galactic nucleus, astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Electromagnetic radiation, symbols.namesake, SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, Nuclear, MASSES, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Active galactic nuclei, Molecular, Astronomy and Astrophysics, Light curve, Astrophysics - Astrophysics of Galaxies, Black hole, CONTINUUM, SIZE, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Active galaxies, EMISSION
Abstract

We present geometric and dynamical modeling of the broad line region for the multi-wavelength reverberation mapping campaign focused on NGC 5548 in 2014. The dataset includes photometric and spectroscopic monitoring in the optical and ultraviolet, covering the H$\beta$, C IV, and Ly$\alpha$ broad emission lines. We find an extended disk-like H$\beta$ BLR with a mixture of near-circular and outflowing gas trajectories, while the C IV and Ly$\alpha$ BLRs are much less extended and resemble shell-like structures. There is clear radial structure in the BLR, with C IV and Ly$\alpha$ emission arising at smaller radii than the H$\beta$ emission. Using the three lines, we make three independent black hole mass measurements, all of which are consistent. Combining these results gives a joint inference of $\log_{10}(M_{\rm BH}/M_\odot) = 7.64^{+0.21}_{-0.18}$. We examine the effect of using the $V$ band instead of the UV continuum light curve on the results and find a size difference that is consistent with the measured UV-optical time lag, but the other structural and kinematic parameters remain unchanged, suggesting that the $V$ band is a suitable proxy for the ionizing continuum when exploring the BLR structure and kinematics. Finally, we compare the H$\beta$ results to similar models of data obtained in 2008 when the AGN was at a lower luminosity state. We find that the size of the emitting region increased during this time period, but the geometry and black hole mass remain unchanged, which confirms that the BLR kinematics suitably gauge the gravitational field of the central black hole., Comment: 26 pages, 19 figures, 1 table, accepted for publication in ApJ

Published
2020

28. Space Telescope and optical reverberation mapping project. XI. Disk-wind characteristics and contributions to the very broad emission lines of NGC 5548

Author

J. M. Gelbord, Bradley M. Peterson, Marianne Vestergaard, E. Dalla Bontà, M. Dehghanian, G. De Rosa, Missagh Mehdipour, Gary J. Ferland, Smita Mathur, Jelle Kaastra, Misty C. Bentz, I. M. McHardy, Marios Chatzikos, Kirk T. Korista, Gerard A. Kriss, Daniel Proga, M. R. Goad, D. A. Starkey, Tim Waters, R. W. Pogge, Michael Fausnaugh, F. Guzmán, Susanna Bisogni, Keith Horne, W. N. Brandt, ITA, USA, GBR, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
ACTIVE GALACTIC NUCLEI, Seyfert [Galaxies], Active galactic nucleus, 010504 meteorology & atmospheric sciences, active [Galaxies], individual (NGC 5548) [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), NDAS, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Spitzer Space Telescope, 0103 physical sciences, QB Astronomy, SPECTRA, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Optical depth, QC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation), QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Active galactic nuclei, Seyfert galaxies, CLOUDS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, QC Physics, 13. Climate action, Space and Planetary Science, nuclei [Galaxies], formation [Line], Astrophysics of Galaxies (astro-ph.GA), BLACK-HOLE, Active galaxies, Reverberation mapping, Astrophysics - High Energy Astrophysical Phenomena
Abstract

In 2014 the NGC 5548 Space Telescope and Optical Reverberation Mapping campaign discovered a two-month anomaly when variations in the absorption and emission lines decorrelated from continuum variations. During this time the soft X-ray part of the intrinsic spectrum had been strongly absorbed by a line-of-sight (LOS) obscurer, which was interpreted as the upper part of a disk wind. Our first paper showed that changes in the LOS obscurer produce the decorrelation between the absorption lines and the continuum. A second study showed that the base of the wind shields the BLR, leading to the emission-line decorrelation. In that study, we proposed the wind is normally transparent with no effect on the spectrum. Changes in the wind properties alter its shielding and affect the SED striking the BLR, producing the observed decorrelations. In this work, we investigate the impact of a translucent wind on the emission lines. We simulate the obscuration using XMM-Newton, NuSTAR, and HST observations to determine the physical characteristics of the wind. We find that a translucent wind can contribute a part of the He II and Fe K? emission. It has a modest optical depth to electron scattering, which explains the fainter far-side emission in the observed velocity delay maps. The wind produces the very broad base seen in the UV emission lines and may also be present in the Fe K? line. Our results highlight the importance of accounting for the effects of such winds in the analysis of the physics of the central engine., Comment: Accepted for publication in ApJ

Published
2020

29. Compact nuclear objects and properties of their parent galaxies.

Author

Zasov, Anatoly V. and Cherepashchuk, Anatoly M.

Abstract

We consider the relationship between the masses of the compact nuclear objects in the centers of disky galaxies – supermassive black holes (SMBHs) or nuclear star clusters (NCs) – and such parameters as the maximal velocity of rotation Vmax, obtained from the rotation curves, indicative dynamical mass M25, and the color index (B−V) of their parent galaxies. It was found that the mass of nuclear clusters Mnc correlates more closely with the velocity of rotation and total mass of galaxies than the mass of supermassive black holes Mbh. The dependence of masses of the central objects on the color index is bimodal: galaxies of the red group (red-sequence), which have (B−V) > 0.6−0.7, differ from bluer galaxies, by higher values of Mbh for similar host-galaxy parameters. In contrast, in the diagrams for nuclear clusters the “blue” and “red” galaxies form unified sequences. It agrees with scenarios in which most red-group galaxies form as a result of loss of interstellar gas in a stage of high nuclear activity in galaxies whose central black-hole masses are high, exceeding 106 − 107M⊙ (depending on the total mass of the galaxy). The active growth of nuclear star clusters possibly begun after the violent AGN activity. [ABSTRACT FROM PUBLISHER]

Published
2013
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30. Two ten-billion-solar-mass black holes at the centres of giant elliptical galaxies.

Author

McConnell, Nicholas J., Ma, Chung-Pei, Gebhardt, Karl, Wright, Shelley A., Murphy, Jeremy D., Lauer, Tod R., Graham, James R., and Richstone, Douglas O.

Subjects
ELLIPTICAL galaxies, QUASARS, BLACK holes, GALAXIES, M87 (Galaxy), UNIVERSE, EARTH (Planet)
Abstract

Observational work conducted over the past few decades indicates that all massive galaxies have supermassive black holes at their centres. Although the luminosities and brightness fluctuations of quasars in the early Universe suggest that some were powered by black holes with masses greater than 10 billion solar masses, the remnants of these objects have not been found in the nearby Universe. The giant elliptical galaxy Messier 87 hosts the hitherto most massive known black hole, which has a mass of 6.3 billion solar masses. Here we report that NGC 3842, the brightest galaxy in a cluster at a distance from Earth of 98 megaparsecs, has a central black hole with a mass of 9.7 billion solar masses, and that a black hole of comparable or greater mass is present in NGC 4889, the brightest galaxy in the Coma cluster (at a distance of 103 megaparsecs). These two black holes are significantly more massive than predicted by linearly extrapolating the widely used correlations between black-hole mass and the stellar velocity dispersion or bulge luminosity of the host galaxy. Although these correlations remain useful for predicting black-hole masses in less massive elliptical galaxies, our measurements suggest that different evolutionary processes influence the growth of the largest galaxies and their black holes. [ABSTRACT FROM AUTHOR]

Published
2011
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32. Space Telescope and Optical Reverberation Mapping Project. VIII. Time Variability of Emission and Absorption in NGC 5548 Based on Modeling the Ultraviolet Spectrum

Author

Andrew J. King, K. G. Teems, Gabriele Ponti, J. S. Schimoia, Calen B. Henderson, Michael S. Brotherton, S. Paltani, Nahum Arav, Alessandro Siviero, Radosław Poleski, P. Lira, Sang Chul Kim, Thomas W.-S. Holoien, Wei Zhu, A. de Lorenzo-Cáceres, M. C. Bottorff, Dirk Grupe, Gabriela Canalizo, M. Eracleous, S. G. Sergeev, F. MacInnis, Massimo Cappi, M. Dietrich, Alis J. Deason, Haojing Yan, Giorgio Matt, Ciro Pinto, Michael T. Carini, Minjin Kim, Brandon C. Kelly, I. M. McHardy, Scott M. Adams, L. Gonzalez, J. J. Jensen, Julia M. Comerford, Yair Krongold, Tim Waters, B. Scott, C. S. Turner, G. A. Borman, R. McGurk, Nicolas Tejos, J. R. Parks, K. Flatland, Michael D. Joner, Kirk T. Korista, L. Di Gesu, Emma Gardner, Jon C. Mauerhan, Jessie C. Runnoe, Douglas C. Leonard, Kelsey I. Clubb, M. H. Siegel, C. A. Johnson, D. A. Starkey, H. Yuk, M. A. Malkan, Justin Ely, Ying Zu, Aaron J. Barth, Cassandra Lochhaas, Patrick L. Kelly, E. Holmbeck, Hyun-Il Sung, Patrick B. Hall, C. Montuori, Christopher S. Kochanek, Bradley M. Peterson, Tommaso Treu, Missagh Mehdipour, Marie Wingyee Lau, A. Skielboe, Catherine J. Grier, J. A. Kennea, Thomas G. Beatty, R. W. Pogge, J. van Saders, A. Bigley, S. Hicks, Catia Silva, H. W. Rix, Vardha N. Bennert, D. M. Crenshaw, E. Dalla Bontà, Miao Li, A. A. Breeveld, Dom Walton, D. N. Okhmat, Elisa Costantini, P. Ochner, Y. Weiss, M. L. Nguyen, Ryan Norris, Susanna Bisogni, Ehud Behar, Jacobo Ebrero, Garrett Somers, Phil Uttley, S. Rafter, Kelly D. Denney, K. Schnülle, Carolin Villforth, Keith Horne, Smita Mathur, G. V. Simonian, R. Boissay-Malaquin, Gary J. Ferland, J. S. Brown, Jelle Kaastra, Ana M. Mosquera, Stefano Bianchi, Misty C. Bentz, A. Pancoast, Alessandro Pizzella, WeiKang Zheng, N. Gehrels, Daniel J. Stevens, M. Dehghanian, Kevin V. Croxall, Isaac Shivvers, A. Gupta, Chris Done, J. E. Brown, B. De Marco, Gerard A. Kriss, Steve Croft, S. V. Nazarov, J. A. Nousek, Jae-Ok Lee, P. Arévalo, G. De Rosa, Michael Fausnaugh, Rick Edelson, Phil Evans, Lorenzo Morelli, S. Geier, Enrico Maria Corsini, M. R. Goad, V. Gorjian, W. N. Brandt, Elinor L. Gates, Shai Kaspi, D. A. Saylor, Jong-Hak Woo, Edward M. Cackett, Liuyi Pei, T. Hutchison, Jamie Tayar, E. R. Manne-Nicholas, Laura Vican, Daniel Proga, Steven Villanueva, D. Mudd, J.-U. Pott, F. Müller-Sánchez, Alexei V. Filippenko, Hagai Netzer, S. A. Klimanov, B. J. Shappee, J. M. Gelbord, Marianne Vestergaard, M. Spencer, Zhiyuan Ma, Carl T. Coker, S. Y. Kim, Myungshin Im, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), Kriss, G. A., De Rosa, G., Ely, J., Peterson, B. M., Kaastra, J., Mehdipour, M., Ferland, G. J., Dehghanian, M., Mathur, S., Edelson, R., Korista, K. T., Arav, N., Barth, A. J., Bentz, M. C., Brandt, W. N., Crenshaw, D. M., Bontà, E. Dalla, Denney, K. D., Done, C., Eracleous, M., Fausnaugh, M. M., Gardner, E., Goad, M. R., Grier, C. J., Horne, Keith, Kochanek, C. S., Mchardy, I. M., Netzer, H., Pancoast, A., Pei, L., Pogge, R. W., Proga, D., Silva, C., Tejos, N., Vestergaard, M., Adams, S. M., Anderson, M. D., Arévalo, P., Beatty, T G., Behar, E., Bennert, V. N., Bianchi, S., Bigley, A., Bisogni, S., Boissay-Malaquin, R., Borman, G. A., Bottorff, M. C., Breeveld, A. A., Brotherton, M., Brown, J. E., Brown, J. S., Cackett, E. M., Canalizo, G., Cappi, M., Carini, M. T., Clubb, K. I., Comerford, J. M., Coker, C. T., Corsini, E. M., Costantini, E., Croft, S., Croxall, K. V., Deason, A. J., De Lorenzo-Cáceres, A., De Marco, B., Dietrich, M., Di Gesu, L., Ebrero, J., Evans, P. A., Filippenko, A. V., Flatland, K., Gates, E. L., Gehrels, N., Geier, S., Gelbord, J. M., Gonzalez, L., Gorjian, V., Grupe, D., Gupta, A., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W. -S., Hutchison, T. A., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Kaspi, S., Kelly, B. C., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S. C., Kim, S. Y., King, A., Klimanov, S. A., Krongold, Y., Lau, M. W., Lee, J. C., Leonard, D. C., Li, Miao, Lira, P., Lochhaas, C., Ma, Zhiyuan, Macinnis, F., Malkan, M. A., Manne-Nicholas, E. R., Matt, G., Mauerhan, J. C., Mcgurk, R., Montuori, C., Morelli, L., Mosquera, A., Mudd, D., Müller-Sánchez, F., Nazarov, S. V., Norris, R. P., Nousek, J. A., Nguyen, M. L., Ochner, P., Okhmat, D. N., Paltani, S., Parks, J. R., Pinto, C., Pizzella, A., Poleski, R., Ponti, G., Pott, J. -U., Rafter, S. E., Rix, H. -W., Runnoe, J., Saylor, D. A., Schimoia, J. S., Schnülle, K., Scott, B., Sergeev, S. G., Shappee, B. J., Shivvers, I., Siegel, M., Simonian, G. V., Siviero, A., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Sung, H. -I., Tayar, J., Teems, K. G., Treu, T., Turner, C. S., Uttley, P., Van Saders, J ., Vican, L., Villforth, C., Villanueva Jr., S., Walton, D. J., Waters, T., Weiss, Y., Woo, J. -H., Yan, H., Yuk, H., Zheng, W., Zhu, W., Zu, Y., and USA

Subjects
Seyfert [Galaxies], galaxies: active, galaxies: individual (NGC 5548), galaxies: nuclei, galaxies: Seyfert, 010504 meteorology & atmospheric sciences, Absorption spectroscopy, active [Galaxies], individual (NGC 5548) [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Luminosity, 0103 physical sciences, QB Astronomy, Emission spectrum, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, Astronomy and Astrophysics, DAS, Astrophysics - Astrophysics of Galaxies, Galaxy, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), nuclei [Galaxies], Reverberation mapping
Abstract

We model the ultraviolet spectra of the Seyfert 1 galaxy NGC~5548 obtained with the Hubble Space Telescope during the 6-month reverberation-mapping campaign in 2014. Our model of the emission from NGC 5548 corrects for overlying absorption and deblends the individual emission lines. Using the modeled spectra, we measure the response to continuum variations for the deblended and absorption-corrected individual broad emission lines, the velocity-dependent profiles of Ly$\alpha$ and C IV, and the narrow and broad intrinsic absorption features. We find that the time lags for the corrected emission lines are comparable to those for the original data. The velocity-binned lag profiles of Ly$\alpha$ and C IV have a double-peaked structure indicative of a truncated Keplerian disk. The narrow absorption lines show delayed response to continuum variations corresponding to recombination in gas with a density of $\sim 10^5~\rm cm^{-3}$. The high-ionization narrow absorption lines decorrelate from continuum variations during the same period as the broad emission lines. Analyzing the response of these absorption lines during this period shows that the ionizing flux is diminished in strength relative to the far-ultraviolet continuum. The broad absorption lines associated with the X-ray obscurer decrease in strength during this same time interval. The appearance of X-ray obscuration in $\sim\,2012$ corresponds with an increase in the luminosity of NGC 5548 following an extended low state. We suggest that the obscurer is a disk wind triggered by the brightening of NGC 5548 following the decrease in size of the broad-line region during the preceding low-luminosity state., Comment: 50 pages, 30 figures, uses aastex62.cls. Accepted for publication in ApJ, 07/06/2019. High-level products page in MAST will go live after 7/15/2019. Replaced Figure 4 on 7/12/2019 to be more red/green color-blind friendly

Published
2019

33. The Cepheid Distance to the Seyfert 1 Galaxy NGC 4151

Author

Bradley M. Peterson, E. Dalla Bontà, Laura Ferrarese, Christopher A. Onken, S. L. Hoffmann, Wenlong Yuan, J. S. Brown, Lucas M. Macri, Ric Davies, E. K. S. Hicks, G. De Rosa, C. J. Grier, Marianne Vestergaard, Thaisa Storchi-Bergmann, Richard W. Pogge, Misty C. Bentz, Adam G. Riess, and Michael Fausnaugh

Subjects
Cepheid variable stars, ACTIVE GALACTIC NUCLEI, Cepheid variable, Astrophysics::High Energy Astrophysical Phenomena, Near infrared astronomy, Galaxy distances, FOS: Physical sciences, Time series analysis, Distance indicators, REVERBERATION MAPPING DATA, MAGNITUDES, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, MASS, GRAVITATIONAL LENSING EXPERIMENT, SUPERMASSIVE BLACK-HOLES, Hubble space telescope, Hubble Space Telescope, Astrophysics::Solar and Stellar Astrophysics, HST photometry, KINEMATICS, OGLE-III CATALOG, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, AGN host galaxies, Physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, NARROW-LINE REGION, Cepheid distance, Astrophysics - Solar and Stellar Astrophysics, GEMINI NIFS, Distance measure, Optical observatories, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract

We derive a distance of $15.8\pm0.4$ Mpc to the archetypical Seyfert 1 galaxy NGC 4151 based on the near-infrared Cepheid Period-Luminosity relation and new Hubble Space Telescope multiband imaging. This distance determination, based on measurements of 35 long-period ($P > 25$d) Cepheids, will support the absolute calibration of the supermassive black hole mass in this system, as well as studies of the dynamics of the feedback or feeding of its active galactic nucleus., 18 pages. 11 figures. 7 tables. Accepted for publication in ApJ

Published
2020

34. THE ROLE of QUENCHING TIME in the EVOLUTION of the MASS-SIZE RELATION of PASSIVE GALAXIES from the WISP SURVEY

Author

Alejandro Bedregal, Christopher Martin, Andrew Bunker, Hakim Atek, E. Dalla Bontà, Claudia Scarlata, Y. S. Dai, Brian Siana, Marc Rafelski, Michael Rutkowski, James W. Colbert, A. Zanella, Alaina Henry, M. Malkan, Enrico Maria Corsini, and Harry I. Teplitz

Subjects
Stellar population, Infrared, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Atomic, Physical Chemistry, Photometry (optics), Particle and Plasma Physics, galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, fundamental parameters [galaxies], Nuclear, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], Physics, galaxies: evolution, galaxies: fundamental parameters, galaxies: structure, Astronomy and Astrophysics, Space and Planetary Science, 010308 nuclear & particles physics, Star formation, Molecular, Radius, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Astrophysics of Galaxies (astro-ph.GA), structure [galaxies], Astrophysics::Earth and Planetary Astrophysics, Wide Field Camera 3, high-redshift [galaxies], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

We analyze how passive galaxies at z $\sim$ 1.5 populate the mass-size plane as a function of their stellar age, to understand if the observed size growth with time can be explained with the appearance of larger quenched galaxies at lower redshift. We use a sample of 32 passive galaxies extracted from the Wide Field Camera 3 Infrared Spectroscopic Parallel (WISP) survey with spectroscopic redshift 1.3 $\lesssim$ z $\lesssim$ 2.05, specific star-formation rates lower than 0.01 Gyr$^{-1}$, and stellar masses above 4.5 $\times$ 10$^{10}$ M$_\odot$. All galaxies have spectrally determined stellar ages from fitting of their rest-frame optical spectra and photometry with stellar population models. When dividing our sample into young (age $\leq$ 2.1 Gyr) and old (age $>$ 2.1 Gyr) galaxies we do not find a significant trend in the distributions of the difference between the observed radius and the one predicted by the mass-size relation. This result indicates that the relation between the galaxy age and its distance from the mass-size relation, if it exists, is rather shallow, with a slope alpha $\gtrsim$ -0.6. At face value, this finding suggests that multiple dry and/or wet minor mergers, rather than the appearance of newly quenched galaxies, are mainly responsible for the observed time evolution of the mass-size relation in passive galaxies., Accepted for publication in ApJ Letters; 6 pages, 3 figures, 1 table

Published
2016

35. Space Telescope and Optical Reverberation Mapping Project. VII. Understanding the Ultraviolet Anomaly in NGC 5548 with X-Ray Spectroscopy

Author

Mathur, S., Gupta, A., Page, K., Pogge, R. W., Krongold, Y., Goad, M. R., Adams, S. M., Anderson, M. D., Arã©valo, P., Barth, A. J., Bazhaw, C., Beatty, T. G., Bentz, M. C., Bigley, A., Bisogni, S., Borman, G. A., Boroson, T. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Brown, J. E., Brown, J. S., Cackett, E. M., Canalizo, G., Carini, M. T., Clubb, K. I., Comerford, J. M., Coker, C. T., Corsini, E. M., Crenshaw, D. M., Croft, S., Croxall, K. V., Dalla Bontã , E., Deason, A. J., Denney, K. D., De Lorenzo-cã¡ceres, A., De Rosa, G., Dietrich, M., Edelson, R., Ely, J., Eracleous, M., Evans, P. A., Fausnaugh, M. M., Ferland, G. J., Filippenko, A. V., Flatland, K., Fox, O. D., Gates, E. L., Gehrels, N., Geier, S., Gelbord, J. M., Gorjian, V., Greene, J. E., Grier, C. J., Grupe, D., Hall, P. B., Henderson, C. B., Hicks, S., Holmbeck, E., Holoien, T. W. -. S., Horenstein, D., Horne, Keith, Hutchison, T., Im, M., Jensen, J. J., Johnson, C. A., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kelly, P. L., Kennea, J. A., Kim, M., Kim, S., Kim, S. C., King, A., Klimanov, S. A., Kochanek, C. S., Korista, K. T., Kriss, G. A., Lau, M. W., Lee, J. C., Leonard, D. C., Li, M., Lira, P., Ma, Z., Macinnis, F., Manne-nicholas, E. R., Malkan, M. A., Mauerhan, J. C., Mcgurk, R., Mchardy, I. M., Montouri, C., Morelli, L., Mosquera, A., Mudd, D., Muller-sanchez, F., Musso, R., Nazarov, S. V., Netzer, H., Nguyen, M. L., Norris, R. P., Nousek, J. A., Ochner, P., Okhmat, D. N., Ou-yang, B., Pancoast, A., Papadakis, I., Parks, J. R., Pei, L., Peterson, B. M., Pizzella, A., Poleski, R., Pott, J. -. U., Rafter, S. E., Rix, H. -. W., Runnoe, J., Saylor, D. A., Schimoia, J. S., Schnã¼lle, K., Sergeev, S. G., Shappee, B. J., Shivvers, I., Siegel, M., Simonian, G. V., Siviero, A., Skielboe, A., Somers, G., Spencer, M., Starkey, D., Stevens, D. J., Sung, H. -. I., Tayar, J., Tejos, N., Turner, C. S., Uttley, P., Van Saders, J., Vestergaard, M., Vican, L., Villanueva, S., Villforth, C., Weiss, Y., Woo, J. -. H., Yan, H., Young, S., Yuk, H., Zheng, W., Zhu, W., Zu, Y., Corsini, ENRICO MARIA, USA, High Energy Astrophys. & Astropart. Phys (API, FNWI), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
active [Galaxies], individual (NGC 5548) [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Continuum (design consultancy), FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, individual (NGC 5548) [X-rays], galaxies: individual (NGC 5548), X-rays: galaxies, X-rays: individual (NGC 5548), Astronomy and Astrophysics, Space and Planetary Science, Spitzer Space Telescope, 0103 physical sciences, QB Astronomy, Emission spectrum, 010303 astronomy & astrophysics, QC, Optical depth, QB, Physics, 010308 nuclear & particles physics, 3rd-DAS, Astrophysics - Astrophysics of Galaxies, galaxies [X-rays], QC Physics, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), Reverberation mapping, Anomaly (physics)
Abstract

During the Space Telescope and Optical Reverberation Mapping Project (STORM) observations of NGC 5548, the continuum and emission-line variability became de-correlated during the second half of the 6-month long observing campaign. Here we present Swift and Chandra X-ray spectra of NGC 5548 obtained as a part of the campaign. The Swift spectra show that excess flux (relative to a power-law continuum) in the soft X-ray band appears before the start of the anomalous emission-line behavior, peaks during the period of the anomaly, and then declines. This is a model-independent result suggesting that the soft excess is related to the anomaly. We divide the Swift data into on- and off-anomaly spectra to characterize the soft excess via spectral fitting. The cause of the spectral differences is likely due to a change in the intrinsic spectrum rather than being due to variable obscuration or partial covering. The Chandra spectra have lower signal-to-noise ratios, but are consistent with Swift data. Our preferred model of the soft excess is emission from an optically thick, warm Comptonizing corona, the effective optical depth of which increases during the anomaly. This model simultaneously explains all the three observations: the UV emission line flux decrease, the soft-excess increase, and the emission line anomaly., ApJ in press. Replaced with the accepted version

Published
2017

37. THE BLACK HOLE–DARK MATTER HALO CONNECTION.

Author

Bassem M. Sabra, Charbel Saliba, Maya Abi Akl, and Gilbert Chahine

Subjects
BLACK holes, DARK matter, STAR observations, GALAXY formation, SPEED measurements
Abstract

We explore the connection between the central supermassive black holes (SMBH) in galaxies and the dark matter halo through the relation between the masses of the SMBHs and the maximum circular velocities of the host galaxies, as well as the relationship between stellar velocity dispersion of the spheroidal component and the circular velocity. Our assumption here is that the circular velocity is a proxy for the mass of the dark matter halo. We rely on a heterogeneous sample containing galaxies of all types. The only requirement is that the galaxy has a direct measurement of the mass of its SMBH and a direct measurement of its circular velocity and its velocity dispersion. Previous studies have analyzed the connection between the SMBH and dark matter halo through the relationship between the circular velocity and the bulge velocity dispersion, with the assumption that the bulge velocity dispersion stands in for the mass of the SMBH, via the well-established SMBH mass–bulge velocity dispersion relation. Using intermediate relations may be misleading when one is studying them to decipher the active ingredients of galaxy formation and evolution. We believe that our approach will provide a more direct probe of the SMBH and the dark matter halo connection. We find that the correlation between the mass of SMBHs and the circular velocities of the host galaxies is extremely weak, leading us to state the dark matter halo may not play a major role in regulating the black hole growth in the present Universe. [ABSTRACT FROM AUTHOR]

Published
2015
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