Physical Sciences and Mathematics Commons^™

Sdss-Iv Manga: Properties Of Galaxies With Kinematically Decoupled Stellar And Gaseous Components, Yifei Jin, Yanmei Chen, Yong Shi, C. A. Tremonti, M. A. Bershady, M. Merrifield, E. Emsellem, Hai Fu, D. Wake, K. Bundy, Lihwai Lin, M. Argudo-Fernandez, Song Huang, D. V. Stark, T. Storchi-Bergmann, D. Bizyaev, J. Brownstein, J. Chisholm, Qi Guo, Lei Hao, Jian Hu, Cheng Li, Ran Li, K. L. Masters, E. Malanushenko, Kaike Pan, R. A. Riffel, A. Roman-Lopes, A. Simmons, D. Thomas, Renbin Yan

Physics and Astronomy Faculty Publications

We study the properties of 66 galaxies with kinematically misaligned gas and stars from MaNGA survey. The fraction of kinematically misaligned galaxies varies with galaxy physical parameters, i.e. M_*, SFR and sSFR. According to their sSFR, we further classify these 66 galaxies into three categories, 10 star-forming, 26 ‘Green Valley’ and 30 quiescent ones. The properties of different types of kinematically misaligned galaxies are different in that the star-forming ones have positive gradient in D_n4000 and higher gas-phase metallicity, while the green valley/quiescent ones have negative D_n4000 gradients and lower gas-phase metallicity on average. …

Interpreting The Ionization Sequence In Star-Forming Galaxy Emission-Line Spectra, Chris T. Richardson, James T. Allen, Jack A. Baldwin, Paul C. Hewett, Gary J. Ferland, Anthony Crider, Helen Meskhidze

Physics and Astronomy Faculty Publications

High-ionization star-forming (SF) galaxies are easily identified with strong emission-line techniques such as the BPT diagram, and form an obvious ionization sequence on such diagrams. We use a locally optimally emitting cloud model to fit emission-line ratios that constrain the excitation mechanism, spectral energy distribution, abundances and physical conditions along the star formation ionization sequence. Our analysis takes advantage of the identification of a sample of pure SF galaxies, to define the ionization sequence, via mean field independent component analysis. Previous work has suggested that the major parameter controlling the ionization level in SF galaxies is the metallicity. Here we …

The Role Of Bulge Formation In The Homogenization Of Stellar Populations At Z ~ 2 As Revealed By Internal Color Dispersion In Candels, Steven Boada, V. Tilvi, R. F. Quadri, M. Hilton, S. Finkelstein, Yicheng Guo, N. Bond, C. Conselice, A. Dekel, H. Ferguson, M. Giavalisco, N. A. Grogin, Dale D. Kocevski, A. M. Koekemoer, D. C. Koo

Physics and Astronomy Faculty Publications

We use data from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey to study how the spatial variation in the stellar populations of galaxies relates to the formation of galaxies at 1.5 < z < 3.5. We use the internal color dispersion (ICD), measured between the rest-frame UV and optical bands, which is sensitive to age (and dust attenuation) variations in stellar populations. The ICD shows a relation with the stellar masses and morphologies of the galaxies. Galaxies with the largest variation in their stellar populations as evidenced by high ICD have disk-dominated morphologies (with Sérsic indexes M/M_⊙) < 11. There is a marked decrease in the ICD as the stellar mass and/or the Sérsic index increases. By studying the relations between the ICD and other galaxy properties including size, total color, star formation rate, and dust attenuation, we conclude that the largest variations in stellar populations occur in galaxies where the light from newly, high star-forming clumps contrasts older stellar disk populations. This phase reaches a peak for galaxies only with a specific stellar mass range, 10 < log(M/M_⊙) < 11, and prior to the formation of a substantial bulge/spheroid. In contrast, galaxies at higher or lower stellar masses and/or higher Sérsic index (n > 2) show reduced ICD values, implying a greater homogeneity of their stellar populations. This indicates that if a galaxy is to have a quiescent bulge along with a star-forming disk, typical of Hubble sequence galaxies, this is most common for stellar masses 10 < log(M/M_⊙) < 11 and when the bulge component remains relatively small (n > 2).

Zfourge/Candels: On The Evolution Of M* Galaxy Progenitors From Z=3 To 0.5*, C. Papovich, I. Labbé, R. Quadri, V. Tilvi, P. Behroozi, E. F. Bell, K. Glazebrook, L. Spitler, C. M.S. Straatman, K.-V. Tran, M. Cowley, R. Davé, A. Dekel, M. Dickinson, H. C. Ferguson, S. L. Finkelstein, E. Gawiser, H. Inami, S. M. Faber, G. G. Kacprzak, L. Kawinwanichakij, Dale D. Kocevski, A. Koekemoer, D. C. Koo, P. Kurczynski, J. M. Lotz, Y. Lu, R. A. Lucas, D. Mcintosh, N. Mehrtens, B. Mobasher, A. Monson, G. Morrison, T. Nanayakkara, S. E. Persson, B. Salmon, R. Simons, A. Tomczak, P. Van Dokkum, B. Weiner, S. P. Willner

Physics and Astronomy Faculty Publications

Galaxies with stellar masses near M* contain the majority of stellar mass in the universe, and are therefore of special interest in the study of galaxy evolution. The Milky Way (MW) and Andromeda (M31) have present-day stellar masses near M*, at 5 × 10¹⁰ M _☉ (defined here to be MW-mass) and 10¹¹ M _☉ (defined to be M31-mass). We study the typical progenitors of these galaxies using the FOURSTAR Galaxy Evolution Survey (ZFOURGE). ZFOURGE is a deep medium-band near-IR imaging survey, which is sensitive to the progenitors of these galaxies out to z ~ 3. …

No More Active Galactic Nuclei In Clumpy Disks Than In Smooth Galaxies At Z ~ 2 In Candels/3d-Hst*, Jonathan R. Trump, Guillermo Barro, Stéphanie Juneau, Benjamin J. Weiner, Bin Luo, Gabriel B. Brammer, Eric F. Bell, W. N. Brandt, Avishai Dekel, Yicheng Guo, Philip F. Hopkins, David C. Koo, Dale D. Kocevski, Daniel H. Mcintosh, Ivelina Momcheva, S. M. Faber, Henry C. Ferguson, Norman A. Grogin, Jeyhan Kartaltepe, Anton M. Koekemoer, Jennifer Lotz, Michael Maseda, Mark Mozena, Kirpal Nandra, David J. Rosario, Gergory R. Zeimann

Physics and Astronomy Faculty Publications

We use CANDELS imaging, 3D-HST spectroscopy, and Chandra X-ray data to investigate if active galactic nuclei (AGNs) are preferentially fueled by violent disk instabilities funneling gas into galaxy centers at 1.3 < z < 2.4. We select galaxies undergoing gravitational instabilities using the number of clumps and degree of patchiness as proxies. The CANDELS visual classification system is used to identify 44 clumpy disk galaxies, along with mass-matched comparison samples of smooth and intermediate morphology galaxies. We note that despite being mass-matched and having similar star formation rates, the smoother galaxies tend to be smaller disks with more prominent bulges compared to the clumpy galaxies. The lack of smooth extended disks is probably a general feature of the z ~ 2 galaxy population, and means we cannot directly compare with the clumpy and smooth extended disks observed at lower redshift. We find that z ~ 2 clumpy galaxies have slightly enhanced AGN fractions selected by integrated line ratios (in the mass-excitation method), but the spatially resolved line ratios indicate this is likely due to extended phenomena rather than nuclear AGNs. Meanwhile, the X-ray data show that …

The Inside-Out Growth Of The Most Massive Galaxies At 0.3 < Z < 0.9, Lei Bai, H. K. C. Yee, Renbin Yan, Eve Lee, David G. Gilbank, E. Ellingson, L. F. Barrientos, M. D. Gladders, B. C. Hsieh, I. H. Li

Physics and Astronomy Faculty Publications

We study the surface brightness profiles of a sample of brightest cluster galaxies (BCGs) with 0.3 < z < 0.9.

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Torus And Active Galactic Nucleus Properties Of Nearby Seyfert Galaxies: Results From Fitting Infrared Spectral Energy Distributions And Spectroscopy, Almudena Alonso-Herrero, Almeida Cristina Ramos, Rachel Mason, Ramos Andrés Asensio, Patrick F. Roche, Nancy A. Levenson, Moshe Elitzur, Christopher Packham, José Miguel Rodríguez Espinosa, Stuart Young, Tanio Díaz-Santos, Ana M. Pérez-García

Physics and Astronomy Faculty Publications

We used the CLUMPY torus models and a Bayesian approach to fit the infrared spectral energy distributions and ground-based high angular resolution mid-infrared spectroscopy of 13 nearby Seyfert galaxies. This allowed us to put tight constraints on torus model parameters such as the viewing angle i, the radial thickness of the torus Y, the angular size of the cloud distribution σ_torus, and the average number of clouds along radial equatorial rays N₀. We found that the viewing angle i is not the only parameter controlling the classification of a galaxy into type 1 or …