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902 results on '"Corsini, E M"'

202. The Fornax 3D project: Non-linear colour–metallicity relation of globular clusters

Author

Fahrion, K., primary, Lyubenova, M., additional, Hilker, M., additional, van de Ven, G., additional, Falcón-Barroso, J., additional, Leaman, R., additional, Martín-Navarro, I., additional, Bittner, A., additional, Coccato, L., additional, Corsini, E. M., additional, Gadotti, D. A., additional, Iodice, E., additional, McDermid, R. M., additional, Pinna, F., additional, Sarzi, M., additional, Viaene, S., additional, de Zeeuw, P. T., additional, and Zhu, L., additional

Published
2020
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203. Fornax 3D project: Automated detection of planetary nebulae in the centres of early-type galaxies and first results

Author

Spriggs, T. W., primary, Sarzi, M., additional, Napiwotzki, R., additional, Galán-de Anta, P. M., additional, Viaene, S., additional, Nedelchev, B., additional, Coccato, L., additional, Corsini, E. M., additional, de Zeeuw, P. T., additional, Falcón-Barroso, J., additional, Gadotti, D. A., additional, Iodice, E., additional, Lyubenova, M., additional, Martín-Navarro, I., additional, McDermid, R. M., additional, Pinna, F., additional, van de Ven, G., additional, and Zhu, L., additional

Published
2020
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204. The Fornax 3D project: Globular clusters tracing kinematics and metallicities

Author

Fahrion, K., primary, Lyubenova, M., additional, Hilker, M., additional, van de Ven, G., additional, Falcón-Barroso, J., additional, Leaman, R., additional, Martín-Navarro, I., additional, Bittner, A., additional, Coccato, L., additional, Corsini, E. M., additional, Gadotti, D. A., additional, Iodice, E., additional, McDermid, R. M., additional, Pinna, F., additional, Sarzi, M., additional, Viaene, S., additional, de Zeeuw, P. T., additional, and Zhu, L., additional

Published
2020
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205. Modeling Gas and Stellar Kinematics in Disc Galaxies

Author

Pignatelli, E., primary, Beltrán, J. C. Vega, additional, Beckman, J. E., additional, Corsini, E. M., additional, Pizzella, A., additional, Scarlata, C., additional, Bertola, F., additional, Funes, J. G., additional, and Zeilinger, W. W., additional

Published
2001
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206. AlFoCS + Fornax3D:resolved star formation in the Fornax cluster with ALMA and MUSE

Author

Zabel, N. (N.), Davis, T. A. (T. A.), Sarzi, M. (M.), Nedelchev, B. (Boris), Chevance, M. (M.), Kruijssen, M. D. (M. Diederik), Iodice, E. (E.), Baes, M. (M.), Bendo, G. J. (G. J.), Corsini, E. M. (E. Maria), De Looze, I. (I.), de Zeeuw, P. T. (P. Tim), Gadotti, D. A. (D. A.), Grossi, M. (M.), Peletier, R. (R.), Pinna, F. (F.), Serra, P. (Paolo), van de Voort, F. (F.), Venhola, A. (A.), Viaene, S. (S.), Vlahakis, C. (C.), Zabel, N. (N.), Davis, T. A. (T. A.), Sarzi, M. (M.), Nedelchev, B. (Boris), Chevance, M. (M.), Kruijssen, M. D. (M. Diederik), Iodice, E. (E.), Baes, M. (M.), Bendo, G. J. (G. J.), Corsini, E. M. (E. Maria), De Looze, I. (I.), de Zeeuw, P. T. (P. Tim), Gadotti, D. A. (D. A.), Grossi, M. (M.), Peletier, R. (R.), Pinna, F. (F.), Serra, P. (Paolo), van de Voort, F. (F.), Venhola, A. (A.), Viaene, S. (S.), and Vlahakis, C. (C.)

Abstract

We combine data from ALMA and MUSE to study the resolved (∼300 pc scale) star formation relation (star formation rate, SFR, versus molecular gas surface density) in cluster galaxies. Our sample consists of nine Fornax cluster galaxies, including spirals, ellipticals, and dwarfs, covering a stellar mass range of ∼10⁸.⁸–10¹¹ M⊙. CO(1–0) and extinction corrected Hα were used as tracers for the molecular gas mass and SFR, respectively. We compare our results with Kennicutt and Bigiel et al. Furthermore, we create depletion time maps to reveal small-scale variations in individual galaxies. We explore these further in FCC290, using the ‘uncertainty principle for star formation’ (Kruijssen & Longmore) to estimate molecular cloud lifetimes, which we find to be short (<10 Myr) in this galaxy. Galaxy-averaged depletion times are compared with other parameters such as stellar mass and cluster-centric distance. We find that the star formation relation in the Fornax cluster is close to those from Kennicutt and Bigiel et al., but overlaps mostly with the shortest depletion times predicted by Bigiel et al. This slight decrease in depletion time is mostly driven by dwarf galaxies with disturbed molecular gas reservoirs close to the virial radius. In FCC90, a dwarf galaxy with a molecular gas tail, we find that depletion times are a factor ≳10 higher in its tail than in its stellar body.

Published
2020

214. Fossil group origins

Author

Zarattini, S., primary, Aguerri, J. A. L., additional, Biviano, A., additional, Girardi, M., additional, Corsini, E. M., additional, and D’Onghia, E., additional

Published
2019
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215. 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., primary, De Rosa, G., additional, Ely, J., additional, Peterson, B. M., additional, Kaastra, J., additional, Mehdipour, M., additional, Ferland, G. J., additional, Dehghanian, M., additional, Mathur, S., additional, Edelson, R., additional, Korista, K. T., additional, Arav, N., additional, Barth, A. J., additional, Bentz, M. C., additional, Brandt, W. N., additional, Crenshaw, D. M., additional, Bontà, E. Dalla, additional, Denney, K. D., additional, Done, C., additional, Eracleous, M., additional, Fausnaugh, M. M., additional, Gardner, E., additional, Goad, M. R., additional, Grier, C. J., additional, Horne, Keith, additional, Kochanek, C. S., additional, McHardy, I. M., additional, Netzer, H., additional, Pancoast, A., additional, Pei, L., additional, Pogge, R. W., additional, Proga, D., additional, Silva, C., additional, Tejos, N., additional, Vestergaard, M., additional, Adams, S. M., additional, Anderson, M. D., additional, Arévalo, P., additional, Beatty, T G., additional, Behar, E., additional, Bennert, V. N., additional, Bianchi, S., additional, Bigley, A., additional, Bisogni, S., additional, Boissay-Malaquin, R., additional, Borman, G. A., additional, Bottorff, M. C., additional, Breeveld, A. A., additional, Brotherton, M., additional, Brown, J. E., additional, Brown, J. S., additional, Cackett, E. M., additional, Canalizo, G., additional, Cappi, M., additional, Carini, M. T., additional, Clubb, K. I., additional, Comerford, J. M., additional, Coker, C. T., additional, Corsini, E. M., additional, Costantini, E., additional, Croft, S., additional, Croxall, K. V., additional, Deason, A. J., additional, De Lorenzo-Cáceres, A., additional, De Marco, B., additional, Dietrich, M., additional, Di Gesu, L., additional, Ebrero, J., additional, Evans, P. A., additional, Filippenko, A. V., additional, Flatland, K., additional, Gates, E. L., additional, Gehrels, N., additional, Geier, S., additional, Gelbord, J. M., additional, Gonzalez, L., additional, Gorjian, V., additional, Grupe, D., additional, Gupta, A., additional, Hall, P. B., additional, Henderson, C. B., additional, Hicks, S., additional, Holmbeck, E., additional, Holoien, T. W.-S., additional, Hutchison, T. A., additional, Im, M., additional, Jensen, J. J., additional, Johnson, C. A., additional, Joner, M. D., additional, Kaspi, S., additional, Kelly, B. C., additional, Kelly, P. L., additional, Kennea, J. A., additional, Kim, M., additional, Kim, S. C., additional, Kim, S. Y., additional, King, A., additional, Klimanov, S. A., additional, Krongold, Y., additional, Lau, M. W., additional, Lee, J. C., additional, Leonard, D. C., additional, Li, Miao, additional, Lira, P., additional, Lochhaas, C., additional, Ma, Zhiyuan, additional, MacInnis, F., additional, Malkan, M. A., additional, Manne-Nicholas, E. R., additional, Matt, G., additional, Mauerhan, J. C., additional, McGurk, R., additional, Montuori, C., additional, Morelli, L., additional, Mosquera, A., additional, Mudd, D., additional, Müller-Sánchez, F., additional, Nazarov, S. V., additional, Norris, R. P., additional, Nousek, J. A., additional, Nguyen, M. L., additional, Ochner, P., additional, Okhmat, D. N., additional, Paltani, S., additional, Parks, J. R., additional, Pinto, C., additional, Pizzella, A., additional, Poleski, R., additional, Ponti, G., additional, Pott, J.-U., additional, Rafter, S. E., additional, Rix, H.-W., additional, Runnoe, J., additional, Saylor, D. A., additional, Schimoia, J. S., additional, Schnülle, K., additional, Scott, B., additional, Sergeev, S. G., additional, Shappee, B. J., additional, Shivvers, I., additional, Siegel, M., additional, Simonian, G. V., additional, Siviero, A., additional, Skielboe, A., additional, Somers, G., additional, Spencer, M., additional, Starkey, D., additional, Stevens, D. J., additional, Sung, H.-I., additional, Tayar, J., additional, Teems, K. G., additional, Treu, T., additional, Turner, C. S., additional, Uttley, P., additional, Van Saders, J ., additional, Vican, L., additional, Villforth, C., additional, Villanueva Jr., S., additional, Walton, D. J., additional, Waters, T., additional, Weiss, Y., additional, Woo, J.-H., additional, Yan, H., additional, Yuk, H., additional, Zheng, W., additional, Zhu, W., additional, and Zu, Y., additional

Published
2019
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216. Morbidity following salvage esophagectomy for squamous cell carcinoma: the MD Anderson experience

Author

Mitchell, K G, primary, Nelson, D B, additional, Corsini, E M, additional, Vaporciyan, A A, additional, Antonoff, M B, additional, Mehran, R J, additional, Rice, D C, additional, Roth, J A, additional, Sepesi, B, additional, Walsh, G L, additional, Bhutani, M S, additional, Maru, D M, additional, Wu, C C, additional, Nguyen, Q-N, additional, Ajani, J A, additional, Swisher, S G, additional, and Hofstetter, W L, additional

Published
2019
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218. The Fornax3D project: Tracing the assembly history of the cluster from the kinematic and line-strength maps

Author

Iodice, E., primary, Sarzi, M., additional, Bittner, A., additional, Coccato, L., additional, Costantin, L., additional, Corsini, E. M., additional, van de Ven, G., additional, de Zeeuw, P. T., additional, Falcón-Barroso, J., additional, Gadotti, D. A., additional, Lyubenova, M., additional, Martín-Navarro, I., additional, McDermid, R. M., additional, Nedelchev, B., additional, Pinna, F., additional, Pizzella, A., additional, Spavone, M., additional, and Viaene, S., additional

Published
2019
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219. Fornax 3D project: a two-dimensional view of the stellar initial mass function in the massive lenticular galaxy FCC 167

Author

Martín-Navarro, I., primary, Lyubenova, M., additional, van de Ven, G., additional, Falcón-Barroso, J., additional, Coccato, L., additional, Corsini, E. M., additional, Gadotti, D. A., additional, Iodice, E., additional, La Barbera, F., additional, McDermid, R. M., additional, Pinna, F., additional, Sarzi, M., additional, Viaene, S., additional, de Zeeuw, P. T., additional, and Zhu, L., additional

Published
2019
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220. The Fornax 3D project: Thick disks in a cluster environment

Author

Pinna, F., primary, Falcón-Barroso, J., additional, Martig, M., additional, Coccato, L., additional, Corsini, E. M., additional, de Zeeuw, P. T., additional, Gadotti, D. A., additional, Iodice, E., additional, Leaman, R., additional, Lyubenova, M., additional, Martín-Navarro, I., additional, Morelli, L., additional, Sarzi, M., additional, van de Ven, G., additional, Viaene, S., additional, and McDermid, R. M., additional

Published
2019
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222. The Fornax 3D project: Unveiling the thick disk origin in FCC 170; possible signs of accretion

Author

Pinna, F., primary, Falcón-Barroso, J., additional, Martig, M., additional, Sarzi, M., additional, Coccato, L., additional, Iodice, E., additional, Corsini, E. M., additional, de Zeeuw, P. T., additional, Gadotti, D. A., additional, Leaman, R., additional, Lyubenova, M., additional, McDermid, R. M., additional, Minchev, I., additional, Morelli, L., additional, van de Ven, G., additional, and Viaene, S., additional

Published
2019
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223. The Fornax 3D project: dust mix and gas properties in the centre of early-type galaxy FCC 167

Author

Viaene, S., primary, Sarzi, M., additional, Zabel, N., additional, Coccato, L., additional, Corsini, E. M., additional, Davis, T. A., additional, De Vis, P., additional, de Zeeuw, P. T., additional, Falcón-Barroso, J., additional, Gadotti, D. A., additional, Iodice, E., additional, Lyubenova, M., additional, McDermid, R., additional, Morelli, L., additional, Nedelchev, B., additional, Pinna, F., additional, Spriggs, T. W., additional, and van de Ven, G., additional

Published
2019
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225. Evidence of a fast bar in the weakly-interacting galaxy NGC 4264 with MUSE

Author

Cuomo, V, Corsini, E M, Aguerri, J A L, Debattista, Victor P, Coccato, L, Costantin, L, Bontà, E Dalla, Iodice, E, Méndez-Abreu, J, Morelli, L, Pagotto, I, Pizzella, A, Cuomo, V, Corsini, E M, Aguerri, J A L, Debattista, Victor P, Coccato, L, Costantin, L, Bontà, E Dalla, Iodice, E, Méndez-Abreu, J, Morelli, L, Pagotto, I, and Pizzella, A

Abstract

We present surface photometry and stellar kinematics of NGC 4264, a barred lenticular galaxy in the region of the Virgo Cluster undergoing a tidal interaction with one of its neighbours, NGC 4261. We measured the bar radius (abar = 3.2 ± 0.5 kpc) and strength (Sbar = 0.31 ± 0.04) of NGC 4264 from Sloan Digital Sky Survey imaging and its bar pattern speed (Ωbar = 71 ± 4 km s−1 kpc−1) using the Tremaine-Weinberg method with stellar-absorption integral-field spectroscopy performed with the Multi Unit Spectroscopic Explorer at the Very Large Telescope. We derived the circular velocity (Vcirc = 189 ± 10 km s−1) by correcting the stellar streaming velocity for asymmetric drift and calculated the corotation radius (Rcor = 2.8 ± 0.2 kpc) from the bar pattern speed. Finally, we estimated the bar rotation rate (Rcor/abar = 0.88 ± 0.23). We find that NGC 4264 hosts a strong and large bar extending out to the corotation radius. This means that the bar is rotating as fast as it can like nearly all the other bars measured so far even when the systematic error due to the uncertainty on the disc position angle is taken into account. The accurate measurement of the bar rotation rate allows us to infer that the formation of the bar of NGC 4264 was due to self-generated internal processes and not triggered by the ongoing interaction.

Published
2019

227. Fossil group origins

Author

Corsini, E. M., primary, Morelli, L., additional, Zarattini, S., additional, Aguerri, J. A. L., additional, Costantin, L., additional, D’Onghia, E., additional, Girardi, M., additional, Kundert, A., additional, Méndez-Abreu, J., additional, and Thomas, J., additional

Published
2018
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232. The intrinsic three-dimensional shape of galactic bars

Author

Mendez-Abreu, J., Costantin, L., Aguerri, J. A. L., de Lorenzo-Caceres, A., Corsini, E. M., Mendez-Abreu, J., Costantin, L., Aguerri, J. A. L., de Lorenzo-Caceres, A., and Corsini, E. M.

Abstract

We present the first statistical study on the intrinsic three-dimensional (3D) shape of a sample of 83 galactic bars extracted from the CALIFA survey. We use the galaXYZ code to derive the bar intrinsic shape with a statistical approach. The method uses only the geometric information (ellipticities and position angles) of bars and discs obtained from a multi-component photometric decomposition of the galaxy surface-brightness distributions. We find that bars are predominantly prolate-triaxial ellipsoids (68%), with a small fraction of oblate-triaxial ellipsoids (32%). The typical flattening (intrinsic C/A semiaxis ratio) of the bars in our sample is 0.34, which matches well the typical intrinsic flattening of stellar discs at these galaxy masses. We demonstrate that, for prolate-triaxial bars, the intrinsic shape of bars depends on the galaxy Hubble type and stellar mass (bars in massive S0 galaxies are thicker and more circular than those in less massive spirals). The bar intrinsic shape correlates with bulge, disc, and bar parameters. In particular with the bulge-to-total (B/T) luminosity ratio, disc g-r color, and central surface brightness of the bar, confirming the tight link between bars and their host galaxies. Combining the probability distributions of the intrinsic shape of bulges and bars in our sample we show that 52% (16%) of bulges are thicker (flatter) than the surrounding bar at 1$\sigma$ level. We suggest that these percentages might be representative of the fraction of classical and disc-like bulges in our sample, respectively., Comment: 18 pages, 11 figures, accepted for publication in MNRAS

Published
2018
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233. The Fornax3D project: overall goals, galaxy sample, MUSE data analysis and initial results

Author

Sarzi, M., Iodice, E., Coccato, L., Corsini, E. M., de Zeeuw, P. T., Falcón-Barroso, J., Gadotti, D. A., Lyubenova, M., McDermid, R. M., van de Ven, G., Fahrion, K., Pizzella, A., Zhu, L., Sarzi, M., Iodice, E., Coccato, L., Corsini, E. M., de Zeeuw, P. T., Falcón-Barroso, J., Gadotti, D. A., Lyubenova, M., McDermid, R. M., van de Ven, G., Fahrion, K., Pizzella, A., and Zhu, L.

Abstract

The Fornax cluster provides a uniquely compact laboratory to study the detailed history of early-type galaxies and the role played by environment in driving their evolution and their transformation from late-type galaxies. Using the superb capabilities of the Multi Unit Spectroscopic Explorer on the Very Large Telescope, high-quality integral-field spectroscopic data were obtained for the inner regions of all the bright ($m_B\leq15$) galaxies within the virial radius of Fornax. The stellar haloes of early-type galaxies are also covered out to about four effective radii. State-of-the-art stellar dynamical and population modelling allows to aim in particular at better characterising the disc components of fast-rotating early-type galaxies, constraining radial variations in the stellar initial-mass functions and measuring the stellar age, metallicity, and $\alpha$-element abundance of stellar haloes in cluster galaxies. This paper describes the sample selection, observations, and overall goals of the survey, and provides initial results based on the spectroscopic data, including the detailed characterisation of stellar kinematics and populations to large radii; decomposition of galaxy components directly via their orbital structure; the ability to identify globular clusters and planetary nebulae, and derivation of high-quality emission-line diagnostics in the presence of complex ionised gas., Comment: Accepted for publication in Astronomy & Astrophysics. An high resolution version is available at the following link: https://www.dropbox.com/s/bext14c5udhln8n/F3D_paper.pdf?dl=0

Published
2018
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236. Morpho-kinematic properties of field S0 bulges in the CALIFA survey

Author

Méndez-Abreu, J., primary, Aguerri, J. A. L., additional, Falcón-Barroso, J., additional, Ruiz-Lara, T., additional, Sánchez-Menguiano, L., additional, de Lorenzo-Cáceres, A., additional, Costantin, L., additional, Catalán-Torrecilla, C., additional, Zhu, L., additional, Sánchez-Blazquez, P., additional, Florido, E., additional, Corsini, E. M., additional, Wild, V., additional, Lyubenova, M., additional, van de Ven, G., additional, Sánchez, S. F., additional, Bland-Hawthorn, J., additional, Galbany, L., additional, García-Benito, R., additional, García-Lorenzo, B., additional, Delgado, R. M. González, additional, López-Sánchez, A. R., additional, Marino, R. A., additional, Márquez, I., additional, Ziegler, B., additional, and collaboration, the CALIFA, additional

Published
2017
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237. Space Telescope and Optical Reverberation Mapping Project. VII. Understanding the Ultraviolet Anomaly in NGC 5548 with X-Ray Spectroscopy

Author

Mathur, S., primary, Gupta, A., additional, Page, K., additional, Pogge, R. W., additional, Krongold, Y., additional, Goad, M. R., additional, Adams, S. M., additional, Anderson, M. D., additional, Arévalo, P., additional, Barth, A. J., additional, Bazhaw, C., additional, Beatty, T. G., additional, Bentz, M. C., additional, Bigley, A., additional, Bisogni, S., additional, Borman, G. A., additional, Boroson, T. A., additional, Bottorff, M. C., additional, Brandt, W. N., additional, Breeveld, A. A., additional, Brown, J. E., additional, Brown, J. S., additional, Cackett, E. M., additional, Canalizo, G., additional, Carini, M. T., additional, Clubb, K. I., additional, Comerford, J. M., additional, Coker, C. T., additional, Corsini, E. M., additional, Crenshaw, D. M., additional, Croft, S., additional, Croxall, K. V., additional, Dalla Bontà, E., additional, Deason, A. J., additional, Denney, K. D., additional, De Lorenzo-Cáceres, A., additional, De Rosa, G., additional, Dietrich, M., additional, Edelson, R., additional, Ely, J., additional, Eracleous, M., additional, Evans, P. A., additional, Fausnaugh, M. M., additional, Ferland, G. J., additional, Filippenko, A. V., additional, Flatland, K., additional, Fox, O. D., additional, Gates, E. L., additional, Gehrels, N., additional, Geier, S., additional, Gelbord, J. M., additional, Gorjian, V., additional, Greene, J. E., additional, Grier, C. J., additional, Grupe, D., additional, Hall, P. B., additional, Henderson, C. B., additional, Hicks, S., additional, Holmbeck, E., additional, Holoien, T. W.-S., additional, Horenstein, D., additional, Horne, Keith, additional, Hutchison, T., additional, Im, M., additional, Jensen, J. J., additional, Johnson, C. A., additional, Joner, M. D., additional, Jones, J., additional, Kaastra, J., additional, Kaspi, S., additional, Kelly, B. C., additional, Kelly, P. L., additional, Kennea, J. A., additional, Kim, M., additional, Kim, S., additional, Kim, S. C., additional, King, A., additional, Klimanov, S. A., additional, Kochanek, C. S., additional, Korista, K. T., additional, Kriss, G. A., additional, Lau, M. W., additional, Lee, J. C., additional, Leonard, D. C., additional, Li, M., additional, Lira, P., additional, Ma, Z., additional, MacInnis, F., additional, Manne-Nicholas, E. R., additional, Malkan, M. A., additional, Mauerhan, J. C., additional, McGurk, R., additional, McHardy, I. M., additional, Montouri, C., additional, Morelli, L., additional, Mosquera, A., additional, Mudd, D., additional, Muller-Sanchez, F., additional, Musso, R., additional, Nazarov, S. V., additional, Netzer, H., additional, Nguyen, M. L., additional, Norris, R. P., additional, Nousek, J. A., additional, Ochner, P., additional, Okhmat, D. N., additional, Ou-Yang, B., additional, Pancoast, A., additional, Papadakis, I., additional, Parks, J. R., additional, Pei, L., additional, Peterson, B. M., additional, Pizzella, A., additional, Poleski, R., additional, Pott, J.-U., additional, Rafter, S. E., additional, Rix, H.-W., additional, Runnoe, J., additional, Saylor, D. A., additional, Schimoia, J. S., additional, Schnülle, K., additional, Sergeev, S. G., additional, Shappee, B. J., additional, Shivvers, I., additional, Siegel, M., additional, Simonian, G. V., additional, Siviero, A., additional, Skielboe, A., additional, Somers, G., additional, Spencer, M., additional, Starkey, D., additional, Stevens, D. J., additional, Sung, H.-I., additional, Tayar, J., additional, Tejos, N., additional, Turner, C. S., additional, Uttley, P., additional, Van Saders, J., additional, Vestergaard, M., additional, Vican, L., additional, Villanueva Jr., S., additional, Villforth, C., additional, Weiss, Y., additional, Woo, J.-H., additional, Yan, H., additional, Young, S., additional, Yuk, H., additional, Zheng, W., additional, Zhu, W., additional, and Zu, Y., additional

Published
2017
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241. Space Telescope and Optical Reverberation Mapping Project. V. Optical Spectroscopic Campaign and Emission-line Analysis for NGC 5548

Author

Pei, L., primary, Fausnaugh, M. M., additional, Barth, A. J., additional, Peterson, B. M., additional, Bentz, M. C., additional, De Rosa, G., additional, Denney, K. D., additional, Goad, M. R., additional, Kochanek, C. S., additional, Korista, K. T., additional, Kriss, G. A., additional, Pogge, R. W., additional, Bennert, V. N., additional, Brotherton, M., additional, Clubb, K. I., additional, Dalla Bontà, E., additional, Filippenko, A. V., additional, Greene, J. E., additional, Grier, C. J., additional, Vestergaard, M., additional, Zheng, W., additional, Adams, Scott M., additional, Beatty, Thomas G., additional, Bigley, A., additional, Brown, Jacob E., additional, Brown, Jonathan S., additional, Canalizo, G., additional, Comerford, J. M., additional, Coker, Carl T., additional, Corsini, E. M., additional, Croft, S., additional, Croxall, K. V., additional, Deason, A. J., additional, Eracleous, Michael, additional, Fox, O. D., additional, Gates, E. L., additional, Henderson, C. B., additional, Holmbeck, E., additional, Holoien, T. W.-S., additional, Jensen, J. J., additional, Johnson, C. A., additional, Kelly, P. L., additional, Kim, S., additional, King, A., additional, Lau, M. W., additional, Li, Miao, additional, Lochhaas, Cassandra, additional, Ma, Zhiyuan, additional, Manne-Nicholas, E. R., additional, Mauerhan, J. C., additional, Malkan, M. A., additional, McGurk, R., additional, Morelli, L., additional, Mosquera, Ana, additional, Mudd, Dale, additional, Sanchez, F. Muller, additional, Nguyen, M. L., additional, Ochner, P., additional, Ou-Yang, B., additional, Pancoast, A., additional, Penny, Matthew T., additional, Pizzella, A., additional, Poleski, Radosław, additional, Runnoe, Jessie, additional, Scott, B., additional, Schimoia, Jaderson S., additional, Shappee, B. J., additional, Shivvers, I., additional, Simonian, Gregory V., additional, Siviero, A., additional, Somers, Garrett, additional, Stevens, Daniel J., additional, Strauss, M. A., additional, Tayar, Jamie, additional, Tejos, N., additional, Treu, T., additional, Van Saders, J., additional, Vican, L., additional, Villanueva, S., additional, Yuk, H., additional, Zakamska, N. L., additional, Zhu, W., additional, Anderson, M. D., additional, Arévalo, P., additional, Bazhaw, C., additional, Bisogni, S., additional, Borman, G. A., additional, Bottorff, M. C., additional, Brandt, W. N., additional, Breeveld, A. A., additional, Cackett, E. M., additional, Carini, M. T., additional, Crenshaw, D. M., additional, De Lorenzo-Cáceres, A., additional, Dietrich, M., additional, Edelson, R., additional, Efimova, N. V., additional, Ely, J., additional, Evans, P. A., additional, Ferland, G. J., additional, Flatland, K., additional, Gehrels, N., additional, Geier, S., additional, Gelbord, J. M., additional, Grupe, D., additional, Gupta, A., additional, Hall, P. B., additional, Hicks, S., additional, Horenstein, D., additional, Horne, Keith, additional, Hutchison, T., additional, Im, M., additional, Joner, M. D., additional, Jones, J., additional, Kaastra, J., additional, Kaspi, S., additional, Kelly, B. C., additional, Kennea, J. A., additional, Kim, M., additional, Kim, S. C., additional, Klimanov, S. A., additional, Lee, J. C., additional, Leonard, D. C., additional, Lira, P., additional, MacInnis, F., additional, Mathur, S., additional, McHardy, I. M., additional, Montouri, C., additional, Musso, R., additional, Nazarov, S. V., additional, Netzer, H., additional, Norris, R. P., additional, Nousek, J. A., additional, Okhmat, D. N., additional, Papadakis, I., additional, Parks, J. R., additional, Pott, J.-U., additional, Rafter, S. E., additional, Rix, H.-W., additional, Saylor, D. A., additional, Schnülle, K., additional, Sergeev, S. G., additional, Siegel, M., additional, Skielboe, A., additional, Spencer, M., additional, Starkey, D., additional, Sung, H.-I., additional, Teems, K. G., additional, Turner, C. S., additional, Uttley, P., additional, Villforth, C., additional, Weiss, Y., additional, Woo, J.-H., additional, Yan, H., additional, Young, S., additional, and Zu, Y., additional

Published
2017
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242. Fossil group origins: X. Velocity segregation in fossil systems.

Author

Zarattini, S., Aguerri, J. A. L., Biviano, A., Girardi, M., Corsini, E. M., and D'Onghia, E.

Subjects
VELOCITY, ASTROPHYSICS, FOSSILS
Abstract

Aims. We aim to study how the velocity segregation and the radial profile of the velocity dispersion depend on the prominence of the brightest cluster galaxies (BCGs). Methods. We divided a sample of 102 clusters and groups of galaxies into four bins of magnitude gap between the two brightest cluster members. We then computed the velocity segregation in bins of absolute and relative magnitude. Moreover, for each bin of magnitude gap we computed the radial profile of the velocity dispersion. Results. When using absolute magnitudes, the segregation in velocity is limited to the two brightest bins and no significant difference is found for different magnitude gaps. However, when we use relative magnitudes, a trend appears in the brightest bin: the larger the magnitude gap, the larger the velocity segregation. We also show that this trend is mainly due to the presence, in the brightest bin, of satellite galaxies in systems with small magnitude gaps: in fact, if we study central galaxies and satellites separately, this trend is mitigated and central galaxies are more segregated than satellites for any magnitude gap. A similar result is found in the radial velocity dispersion profiles: a trend is visible in central regions (where the BCGs dominate) but, if we analyse the profile using satellites alone, the trend disappears. In the latter case, the shape of the velocity dispersion profile in the centre of the systems with different magnitude gaps shows three types of behaviour: systems with the smallest magnitude gaps have an almost flat profile from the centre to the external regions; systems with the largest magnitude gaps show a monothonical growth from the low values of the central part to the flat ones in the external regions; and finally, systems with 1.0 <  Δm12 ≤ 1.5 show a profile that peaks in the centre and then decreases towards the external regions. Conclusions. We suggest that two mechanisms could be responsible for the observed differences in the velocity segregation of the BCGs: an earlier formation of systems with a larger magnitude gap or a more centrally concentrated halo. However, the radial profiles of the velocity dispersion confirm that central galaxies are more relaxed, but that the satellite galaxies do not seem to be affected by the magnitude gap. [ABSTRACT FROM AUTHOR]

Published
2019
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243. The intrinsic shape of bulges in the CALIFA survey

Author

Costantin, L., Méndez-Abreu, J., Corsini, E. M., Eliche-Moral, M. C., Tapia, T., Morelli, L., Bontà, E. Dalla, Pizzella, A., Costantin, L., Méndez-Abreu, J., Corsini, E. M., Eliche-Moral, M. C., Tapia, T., Morelli, L., Bontà, E. Dalla, and Pizzella, A.

Abstract

The intrinsic shape of galactic bulges in nearby galaxies provides crucial information to separate bulge types. We intended to derive accurate constraints to the intrinsic shape of bulges to provide new clues on their formation mechanisms and set new limitations for future simulations. We retrieved the intrinsic shape of a sample of CALIFA bulges using a statistical approach. Taking advantage of GalMer numerical simulations of binary mergers we estimated the reliability of the procedure. Analyzing the $i$-band mock images of resulting lenticular remnants, we studied the intrinsic shape of their bulges at different galaxy inclinations. Finally, we introduced a new ($B/A$, $C/A$) diagram to analyze possible correlations between the intrinsic shape and the properties of bulges. We tested the method on simulated lenticular remnants, finding that for galaxies with inclinations $25^{\circ} < \theta < 65^{\circ}$ we can safely derive the intrinsic shape of their bulges. We found that our CALIFA bulges tend to be nearly oblate systems (66%), with a smaller fraction of prolate spheroids (19%) and triaxial ellipsoids (15%). The majority of triaxial bulges are in barred galaxies (75%). Moreover, we found that bulges with low S\'ersic indices or in galaxies with low bulge-to-total luminosity ratios form a heterogeneous class of objects; additionally, also bulges in late-type galaxies or in less massive galaxies have no preference in being oblate, prolate, or triaxial. On the contrary, bulges with high S\'ersic index, in early-type galaxies, or in more massive galaxies are mostly oblate systems. We concluded that various evolutionary pathways may coexist in galaxies, with merging events and dissipative collapse being the main mechanisms driving the formation of the most massive oblate bulges and bar evolution reshaping the less massive triaxial bulges.

Published
2017
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244. Stringent limits on the masses of the supermassive black holes in seven nearby galaxies

Author

Pagotto, I., Corsini, E. M., Bontà, E. Dalla, Beifiori, A., Costantin, L., Cuomo, V., Morelli, L., Pizzella, A., Sarzi, M., Pagotto, I., Corsini, E. M., Bontà, E. Dalla, Beifiori, A., Costantin, L., Cuomo, V., Morelli, L., Pizzella, A., and Sarzi, M.

Abstract

We present new stringent limits on the mass $M_{bh}$ of the central supermassive black hole for a sample of 7 nearby galaxies. Our $M_{bh}$ estimates are based on the dynamical modeling of the central width of the nebular emission lines measured over subarcsecond apertures with the Hubble Space Telescope. The central stellar velocity dispersion $\sigma_c$ of the sample galaxies is derived from new long-slit spectra from ground-based observations and the bulge effective radius is obtained from a two-dimensional photometric decomposition of the i-band images from the Sloan Digital Sky Survey. The derived stringent $M_{bh}$ limits run parallel and above the $M_{bh}-\sigma_c$ relation with no systematic trend depending on the galaxy distance or morphology. This gives further support to previous findings suggesting that the nuclear gravitational potential is remarkably well traced by the width of the nebular lines when the gas is centrally peaked. With our investigation, the number of galaxies with stringent $M_{bh}$ limits obtained from nebular-line width increases to 114 and can be used for studying the scaling relations between $M_{bh}$ and properties of their host galaxies., Comment: 13 pages, 8 figures, AN in press

Published
2017
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245. Morpho-kinematic properties of field S0 bulges in the CALIFA survey

Author

Mendez-Abreu, J., Aguerri, J. A. L., Falcon-Barroso, J., Ruiz-Lara, T., Sanchez-Menguiano, L., de Lorenzo-Caceres, A., Costantin, L., Catalan-Torrecilla, C., Zhu, L., Sanchez-Blazquez, P., Florido, E., Corsini, E. M., Wild, V., Lyubenova, M., van de Ven, G., Sanchez, S. F., Bland-Hawthorn, J., Galbany, L., Garcia-Benito, R., Garcia-Lorenzo, B., Delgado, R. M. Gonzalez, Lopez-Sanchez, A. R., Marino, R. A., Marquez, I., Ziegler, B., Mendez-Abreu, J., Aguerri, J. A. L., Falcon-Barroso, J., Ruiz-Lara, T., Sanchez-Menguiano, L., de Lorenzo-Caceres, A., Costantin, L., Catalan-Torrecilla, C., Zhu, L., Sanchez-Blazquez, P., Florido, E., Corsini, E. M., Wild, V., Lyubenova, M., van de Ven, G., Sanchez, S. F., Bland-Hawthorn, J., Galbany, L., Garcia-Benito, R., Garcia-Lorenzo, B., Delgado, R. M. Gonzalez, Lopez-Sanchez, A. R., Marino, R. A., Marquez, I., and Ziegler, B.

Abstract

We study a sample of 28 S0 galaxies extracted from the integral-field spectroscopic (IFS) survey CALIFA. We combine an accurate two-dimensional (2D) multi-component photometric decomposition with the IFS kinematic properties of their bulges to understand their formation scenario. Our final sample is representative of S0s with high stellar masses ($M_{star}/M_{sun} > 10^{10}$). They lay mainly on the red sequence and live in relatively isolated environments similar to that of the field and loose groups. We use our 2D photometric decomposition to define the size and photometric properties of the bulges, as well as their location within the galaxies. We perform mock spectroscopic simulations mimicking our observed galaxies to quantify the impact of the underlying disc on our bulge kinematic measurements ($\lambda$ and $v/\sigma$). We compare our bulge corrected kinematic measurements with the results from Schwarzschild dynamical modelling. The good agreement confirms the robustness of our results and allows us to use bulge reprojected values of $\lambda$ and $v/\sigma$. We find that the photometric ($n$ and $B/T$) and kinematic ($v/\sigma$ and $\lambda$) properties of our field S0 bulges are not correlated. We demonstrate that this morpho-kinematic decoupling is intrinsic to the bulges and it is not due to projection effects. We conclude that photometric diagnostics to separate different types of bulges (disc-like vs classical) might not be useful for S0 galaxies. The morpho-kinematics properties of S0 bulges derived in this paper suggest that they are mainly formed by dissipation processes happening at high redshift, but dedicated high-resolution simulations are necessary to better identify their origin., Comment: 31 pages, 19 figures. Accepted for publication in MNRAS

Published
2017
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246. No evidence for small disk-like bulges in a sample of late-type spirals

Author

Costantin, L., Méndez-Abreu, J., Corsini, E. M., Morelli, L., Aguerri, J. A. L., Bontà, E. Dalla, Pizzella, A., Costantin, L., Méndez-Abreu, J., Corsini, E. M., Morelli, L., Aguerri, J. A. L., Bontà, E. Dalla, and Pizzella, A.

Abstract

About 20% of low-redshift galaxies are late-type spirals with a small or no bulge component. Although they are the simplest disk galaxies in terms of structure and dynamics, the role of the different physical processes driving their formation and evolution is not yet fully understood. We investigated whether small bulges of late-type spirals follow the same scaling relations traced by ellipticals and large bulges and if they are disk-like or classical bulges. We derived the photometric and kinematic properties of 9 nearby late-type spirals. To this aim, we analyzed the surface brightness distribution from the i-band images of the Sloan Digital Sky Survey and obtained the structural parameters of the galaxies from a two-dimensional photometric decomposition. We measured the line-of-sight stellar velocity distribution within the bulge effective radius from the long-slit spectra taken with high spectral resolution at the Telescopio Nazionale Galileo. We used the photometric and kinematic properties of the sample bulges to study their location in the Fundamental Plane, Kormendy, and Faber-Jackson relations defined for ellipticals and large bulges. We found that our sample bulges satisfy some of the photometric and kinematic prescriptions for being considered disk-like bulges such as small sizes and masses with nearly exponential light profiles, small bulge-to-total luminosity ratios, low stellar velocity dispersions, and ongoing star formation. However, each of them follows the same scaling relations of ellipticals, massive bulges, and compact early-type galaxies so they cannot be classified as disk-like systems. We find a single population of galaxy spheroids that follow the same scaling relations, where the mass seems to lead to a smooth transition in the photometric and kinematic properties from less massive bulges to more massive bulges and ellipticals., Comment: Accepted for publication in A&A, 20 pages, 10 figures

Published
2017
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247. Space Telescope and Optical Reverberation Mapping Project. VII. Understanding the UV 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., Arevalo, 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., Bonta, E. Dalla, Deason, A. J., Denney, K. D., De Lorenzo-Caceres, 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., Schnülle, 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., VillanuevaJr., S., Villforth, C., Weiss, Y., Woo, J. -H., Yan, H., Young, S., Yuk, H., Zheng, W., Zhu, W., Zu, Y., Mathur, S., Gupta, A., Page, K., Pogge, R. W., Krongold, Y., Goad, M. R., Adams, S. M., Anderson, M. D., Arevalo, 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., Bonta, E. Dalla, Deason, A. J., Denney, K. D., De Lorenzo-Caceres, 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., Schnülle, 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., VillanuevaJr., S., Villforth, C., Weiss, Y., Woo, J. -H., Yan, H., Young, S., Yuk, H., Zheng, W., Zhu, W., and Zu, Y.

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., Comment: ApJ in press. Replaced with the accepted version

Published
2017
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248. Kinematic and stellar population properties of the counter-rotating components in the S0 galaxy NGC 1366

Author

Morelli, L., Pizzella, A., Coccato, L., Corsini, E. M., Bontà, E. Dalla, Buson, L. M., Ivanov, V. D., Pagotto, I., Pompei, E., Rocco, M., Morelli, L., Pizzella, A., Coccato, L., Corsini, E. M., Bontà, E. Dalla, Buson, L. M., Ivanov, V. D., Pagotto, I., Pompei, E., and Rocco, M.

Abstract

Context. Many disk galaxies host two extended stellar components that rotate in opposite directions. The analysis of the stellar populations of the counter-rotating components provides constraints on the environmental and internal processes that drive their formation. Aims. The S0 NGC 1366 in the Fornax cluster is known to host a stellar component that is kinematically decoupled from the main body of the galaxy. Here we successfully separated the two counter-rotating stellar components to independently measure the kinematics and properties of their stellar populations. Methods. We performed a spectroscopic decomposition of the spectrum obtained along the galaxy major axis and separated the relative contribution of the two counter-rotating stellar components and of the ionized-gas component. We measured the line-strength indices of the two counter-rotating stellar components and modeled each of them with single stellar population models that account for the {\alpha}/Fe overabundance. Results. We found that the counter-rotating stellar component is younger, has nearly the same metallicity, and is less {\alpha}/Fe enhanced than the corotating component. Unlike most of the counter-rotating galaxies, the ionized gas detected in NGC 1366 is neither associated with the counter-rotating stellar component nor with the main galaxy body. On the contrary, it has a disordered distribution and a disturbed kinematics with multiple velocity components observed along the minor axis of the galaxy. Conclusions. The different properties of the counter-rotating stellar components and the kinematic peculiarities of the ionized gas suggest that NGC 1366 is at an intermediate stage of the acquisition process, building the counter-rotating components with some gas clouds still falling onto the galaxy., Comment: A&A in press. 8 pages, 6 figures, 2 Table

Published
2017
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249. 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., Kriss, G. A., Pogge, R. W., Bennert, V. N., Brotherton, M., Clubb, K. I., Bontà, E. Dalla, 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., Comerford, J. M., Coker, Carl T., Corsini, E. M., Croft, S., Croxall, K. V., Deason, A. J., Eracleous, Michael, Fox, O. D., Gates, E. L., Henderson, C. B., Holmbeck, E., Holoien, T. W. -S., Jensen, J. J., Johnson, C. A., Kelly, P. L., Kim, S., King, A., Lau, M. W., Li, Miao, 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, Radosław, Runnoe, Jessie, Scott, B., Schimoia, Jaderson S., Shappee, B. J., Shivvers, I., Simonian, Gregory V., Siviero, A., Somers, Garrett, Stevens, Daniel J., Strauss, M. A., Tayar, Jamie, Tejos, N., Treu, T., Van Saders, J., Vican, L., Villanueva Jr., S., Yuk, H., Zakamska, N. L., Zhu, W., Anderson, M. D., Arévalo, P., Bazhaw, C., Bisogni, S., Borman, G. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Cackett, E. M., Carini, M. T., Crenshaw, D. M., De Lorenzo-Cáceres, 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., Horne, Keith, Hutchison, T., Im, M., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kennea, J. A., Kim, M., Kim, S. C., Klimanov, S. A., Lee, J. C., Leonard, D. C., Lira, P., MacInnis, F., Mathur, S., McHardy, I. M., Montouri, C., Musso, R., Nazarov, S. V., Netzer, H., Norris, R. P., Nousek, J. A., Okhmat, D. N., Papadakis, I., Parks, J. R., Pott, J. -U., Rafter, S. E., Rix, H. -W., Saylor, D. A., Schnülle, K., Sergeev, S. G., Siegel, M., Skielboe, A., Spencer, M., Starkey, D., Sung, H. -I., Teems, K. G., Turner, C. S., Uttley, P., Villforth, C., Weiss, Y., Woo, J. -H., Yan, H., Young, S., Zu, 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., Kriss, G. A., Pogge, R. W., Bennert, V. N., Brotherton, M., Clubb, K. I., Bontà, E. Dalla, 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., Comerford, J. M., Coker, Carl T., Corsini, E. M., Croft, S., Croxall, K. V., Deason, A. J., Eracleous, Michael, Fox, O. D., Gates, E. L., Henderson, C. B., Holmbeck, E., Holoien, T. W. -S., Jensen, J. J., Johnson, C. A., Kelly, P. L., Kim, S., King, A., Lau, M. W., Li, Miao, 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, Radosław, Runnoe, Jessie, Scott, B., Schimoia, Jaderson S., Shappee, B. J., Shivvers, I., Simonian, Gregory V., Siviero, A., Somers, Garrett, Stevens, Daniel J., Strauss, M. A., Tayar, Jamie, Tejos, N., Treu, T., Van Saders, J., Vican, L., Villanueva Jr., S., Yuk, H., Zakamska, N. L., Zhu, W., Anderson, M. D., Arévalo, P., Bazhaw, C., Bisogni, S., Borman, G. A., Bottorff, M. C., Brandt, W. N., Breeveld, A. A., Cackett, E. M., Carini, M. T., Crenshaw, D. M., De Lorenzo-Cáceres, 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., Horne, Keith, Hutchison, T., Im, M., Joner, M. D., Jones, J., Kaastra, J., Kaspi, S., Kelly, B. C., Kennea, J. A., Kim, M., Kim, S. C., Klimanov, S. A., Lee, J. C., Leonard, D. C., Lira, P., MacInnis, F., Mathur, S., McHardy, I. M., Montouri, C., Musso, R., Nazarov, S. V., Netzer, H., Norris, R. P., Nousek, J. A., Okhmat, D. N., Papadakis, I., Parks, J. R., Pott, J. -U., Rafter, S. E., Rix, H. -W., Saylor, D. A., Schnülle, K., Sergeev, S. G., Siegel, M., Skielboe, A., Spencer, M., Starkey, D., Sung, H. -I., Teems, K. G., Turner, C. S., Uttley, P., Villforth, C., Weiss, Y., Woo, J. -H., Yan, H., Young, S., and Zu, Y.

Abstract

We present the results of an optical spectroscopic monitoring program targeting NGC 5548 as part of a larger multi-wavelength reverberation mapping campaign. The campaign spanned six months and achieved an almost daily cadence with observations from five ground-based telescopes. The H$\beta$ and He II $\lambda$4686 broad emission-line light curves lag that of the 5100 $\AA$ optical continuum by $4.17^{+0.36}_{-0.36}$ days and $0.79^{+0.35}_{-0.34}$ days, respectively. The H$\beta$ lag relative to the 1158 $\AA$ ultraviolet continuum light curve measured by the Hubble Space Telescope is roughly $\sim$50% longer than that measured against the optical continuum, and the lag difference is consistent with the observed lag between the optical and ultraviolet continua. This suggests that the characteristic radius of the broad-line region is $\sim$50% larger than the value inferred from optical data alone. We also measured velocity-resolved emission-line lags for H$\beta$ and found a complex velocity-lag structure with shorter lags in the line wings, indicative of a broad-line region dominated by Keplerian motion. The responses of both the H$\beta$ and He II $\lambda$4686 emission lines to the driving continuum changed significantly halfway through the campaign, a phenomenon also observed for C IV, Ly $\alpha$, He II(+O III]), and Si IV(+O IV]) during the same monitoring period. Finally, given the optical luminosity of NGC 5548 during our campaign, the measured H$\beta$ lag is a factor of five shorter than the expected value implied by the $R_\mathrm{BLR} - L_\mathrm{AGN}$ relation based on the past behavior of NGC 5548., Comment: 22 pages, 13 figures, accepted to ApJ

Published
2017
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250. Stellar populations of the bulges of four spiral galaxies

Author

Morelli, L., Pizzella, A., Corsini, E. M., Bontà, E. Dalla, Coccato, L., Méndez-Abreu, J., and Parmiggiani, M.

Subjects
Galaxies: bulges, Galaxies: abundances, Galaxies: evolution, FOS: Physical sciences, Astronomy and Astrophysics, ESO-LV 4500200, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, Galaxies: stellar content, Astrophysics - Astrophysics of Galaxies, Galaxies: individual (ESO-LV 1890070, ESO-LV 4460170, ESO-LV 4500200, ESO-LV 5140100), Space and Planetary Science, ESO-LV 4460170, Astrophysics of Galaxies (astro-ph.GA), Galaxies: individual (ESO-LV 1890070, ESO-LV 5140100), Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Key information to understand the formation and evolution of disk galaxies are imprinted in the stellar populations of their bulges. This paper has the purpose to make available new measurements of the stellar population properties of the bulges of four spiral galaxies. Both the central values and radial profiles of the line strength of some of the most common Lick indices are measured along the major- and minor- axis of the bulge-dominated region of the sample galaxies. The corresponding age, metallicity, and {\alpha}/Fe ratio are derived by using the simple stellar population synthesis model predictions. The central values and the gradients of the stellar population properties of ESO-LV1890070, ESO-LV4460170, and ESO-LV 5140100 are consistent with previous findings for bulges of spiral galaxies. On the contrary, the bulge of ESO-LV 4500200 shows peculiar chemical properties possibly due to the presence of a central kinematically-decoupled component. The negative metallicity gradient found in our bulges sample indicates a relevant role for the dissipative collapse in bulge formation. However, the shallow gradients found for the age and {\alpha}/Fe ratio suggests that merging can not be completely ruled out for the sample bulges. This is confirmed by the properties of ESO-LV 4500200 which can hardly be explained without invoking the capture of external material., Comment: 11 pages. 7 figures, AN in press. arXiv admin note: text overlap with arXiv:1203.4284

Published
2015
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