OVERVIEW OF THE SDSS-IV MaNGA SURVEY: MAPPING NEARBY GALAXIES AT APACHE POINT OBSERVATORY

Bundy, Kevin; Bershady, Matthew A.; Law, David R.; Yan, Renbin; Drory, Niv; MacDonald, Nicholas; Wake, David A.; Cherinka, Brian; Sánchez-Gallego, José R.; Weijmans, Anne-Marie; Thomas, Daniel; Tremonti, Christy; Masters, Karen L.; Coccato, L.; Diamond‐Stanic, Aleksandar M.; Aragón-Salamanca, Alfonso; Avila-Reese, Vladimir; Badenes, Carles; Falcón-Barroso, J.; Belfiore, Francesco; Bizyaev, Dmitry; Blanc, Guillermo A.; Bland-Hawthorn, Joss; Blanton, Michael R.; Brownstein, Joel R.; Byler, Nell; Cappellari, Michele; Conroy, Charlie; Dutton, Aaron A.; Emsellem, Éric; Etherington, James; Frinchaboy, Peter M.; Fu, Hai; Gunn, James E.; Harding, Paul; Johnston, Evelyn J.; Kauffmann, Guinevere; Kinemuchi, Karen; Klaene, Mark A.; Knapen, Johan H.; Leauthaud, Alexie; Li, Cheng; Lin, Lihwai; Maiolino, R.; Malanushenko, Viktor; Malanushenko, Elena; Mao, Shude; Maraston, Claudia; McDermid, Richard M.; Merrifield, M. R.; Nichol, R. C.; Oravetz, Daniel; Pan, Kaike; Parejko, John K.; Sanchez, Sebastian Francisco Sanchez; Schlegel, David J.; Simmons, Audrey; Steele, Oliver; Steinmetz, Matthias; Thanjavur, Karun; Thompson, Benjamin; Tinker, Jeremy L.; Bosch, Remco C. E. van den; Westfall, Kyle B.; Wilkinson, David M.; Wright, Shelley A.; Xiao, Ting; Zhang, Kai

doi:10.1088/0004-637x/798/1/7

Cited by 1,525 publications

(1,202 citation statements)

References 103 publications

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“…We can not comment on whether this behaviour extends to lower luminosity galaxies because we are limited by the SDSS spectral resolution. The MaNGA survey (Mapping Nearby Galaxies at Apache Point Observatory, Bundy et al (2015)) plans to obtain integral-field spectroscopy of a representative sample of about 10,000 galaxies above stellar masses of 10 9 M⊙ with redshift around 0.03. Considering the fairly large fraction of galaxies with boxy Hα profiles in massive galaxies, we should expect to see the Hα holes in a substantial fraction of MaNGA galaxies.…”

Section: Discussionmentioning

confidence: 99%

Boxy Hα emission profiles in star-forming galaxies

Chen

Tremonti

et al. 2016

Mon. Not. R. Astron. Soc.

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We assemble a sample of disk star-forming galaxies from the Sloan Digital Sky Survey Data Release 7, studying the structure of Hα emission lines, finding a large fraction of this sample contains boxy Hα line profiles. This fraction depends on galaxy physical and geometric parameters in the following way: (1) it increases monotonically with star formation rate per unit area (Σ SFR ), and stellar mass (M * ), with the trend being much stronger with M * , from ∼0% at M * = 10 10 M ⊙ to about 50% at M * = 10 11 M ⊙ ; (2) the fraction is much smaller in face-on systems than in edge-on systems. It increases with galaxy inclination (i) while i < 60 • and is roughly a constant of 25% beyond this range; (3) for the sources which can be modeled well with two velocity components, blueshifted and redshifted from the systemic velocity, these is a positive correlation between the velocity difference of these two components and the stellar mass, with a slope similar to the Tully-Fisher relation; (4) the two components are very symmetric in the mean, both in velocity and in amplitude. The four findings listed above can be understood as a natural result of a rotating galaxy disk with a kpc-scale ring-like Hα emission region.

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Section: Discussionmentioning

confidence: 99%

Boxy Hα emission profiles in star-forming galaxies

Chen

Tremonti

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The presence of both quasar and radio modes is supported by recent observations. In particular, using MaNGA data (Bundy et al 2015), Cheung et al (2016) report the presence of bi-symmetric emission features in the centre of quiescent galaxies of mass around 2×10 10 M⊙ from which they infer the presence of centrally driven winds. On top of the fact that such "red geysers" galaxies seem to be very common at this mass scale (Bundy et al, in prep), the energy released by their SMBHs is capable of driving the observed winds and displays a mechanical content sufficient to suppress star formation.…”

Section: The Three Simulations Hagn Hnoagn and Hdmmentioning

confidence: 99%

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Peirani

Dubois

Volonteri

et al. 2017

Monthly Notices of the Royal Astronomical Society

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147

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Using a suite of three large cosmological hydrodynamical simulations, HORIZON-AGN, HORIZON-NOAGN (no AGN feedback) and HORIZON-DM (no baryons), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the inner density profiles of massive dark matter haloes and galaxies. Based on direct object-to-object comparisons, we find that the integrated inner mass and density slope differences between objects formed in these three simulations (hereafter, H AGN , H noAGN and H DM ) significantly evolve with time. More specifically, at high redshift (z ∼ 5), the mean central density profiles of H AGN and H noAGN dark matter haloes tend to be much steeper than their H DM counterparts owing to the rapidly growing baryonic component and ensuing adiabatic contraction. By z ∼ 1.5, these mean halo density profiles in H AGN have flattened, pummelled by powerful AGN activity ("quasar mode"): the integrated inner mass difference gaps with H noAGN haloes have widened, and those with H DM haloes have narrowed. Fast forward 9.5 billion years, down to z = 0, and the trend reverses: H AGN halo mean density profiles drift back to a more cusped shape as AGN feedback efficiency dwindles ("radio mode"), and the gaps in integrated central mass difference with H noAGN and H DM close and broaden respectively. On the galaxy side, the story differs noticeably. Averaged stellar profile central densities and inner slopes are monotonically reduced by AGN activity as a function of cosmic time, resulting in better agreement with local observations.

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“…See Bundy et al (2015) for an overview of the MaNGA survey. For a further description of the instrumentation used by MaNGA see Drory et al (2015).…”

Section: Manga Survey and Data Reduction Pipelinementioning

confidence: 99%

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

Smethurst

Masters

Lintott

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Do the theorised different formation mechanisms of fast and slow rotators produce an observable difference in their star formation histories? To study this we identify quenching slow rotators in the MaNGA sample by selecting those which lie below the star forming sequence and identify a sample of quenching fast rotators which were matched in stellar mass. This results in a total sample of 194 kinematically classified galaxies, which is agnostic to visual morphology. We use u − r and N U V − u colours from SDSS and GALEX and an existing inference package, starpy, to conduct a first look at the onset time and exponentially declining rate of quenching of these galaxies. An Anderson-Darling test on the distribution of the inferred quenching rates across the two kinematic populations reveals they are statistically distinguishable (3.2σ). We find that fast rotators quench at a much wider range of rates than slow rotators, consistent with a wide variety of physical processes such as secular evolution, minor mergers, gas accretion and environmentally driven mechanisms. Quenching is more likely to occur at rapid rates (τ ∼ < 1 Gyr) for slow rotators, in agreement with theories suggesting slow rotators are formed in dynamically fast processes, such as major mergers. Interestingly, we also find that a subset of the fast rotators quench at these same rapid rates as the bulk of the slow rotator sample. We therefore discuss how the total gas mass of a merger, rather than the merger mass ratio, may decide a galaxy's ultimate kinematic fate.

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OVERVIEW OF THE SDSS-IV MaNGA SURVEY: MAPPING NEARBY GALAXIES AT APACHE POINT OBSERVATORY

Cited by 1,525 publications

References 103 publications

Boxy Hα emission profiles in star-forming galaxies

Boxy Hα emission profiles in star-forming galaxies

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

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