The ultraviolet upturn in brightest cluster galaxies

Loubser, S. I.; Sánchez‐Blázquez, P.

doi:10.1111/j.1365-2966.2010.17666.x

Cited by 31 publications

(32 citation statements)

References 73 publications

(107 reference statements)

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“…Dust was not observed in the central region of NGC 1453 in our WFC3 data. The mean optical and UV colors of NGC1453 are typical of those of evolved, red giant ellipticals of similar masses (e.g., Faber et al 1989;Loubser & Snchez-Blzquez 2011). Annibali et al (2007) derived a mean age of 9.4 +/-2.1 Gyr and metallicity [Z/H] = +0.22 dex within the central 3".…”

Section: Photometric Datamentioning

confidence: 99%

The MASSIVE Survey. XV. A Stellar Dynamical Mass Measurement of the Supermassive Black Hole in Massive Elliptical Galaxy NGC 1453

Liepold

Quenneville

et al. 2020

ApJ

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We present a new stellar dynamical mass measurement (M BH ) of the supermassive black hole (SMBH) in NGC 1453, a fast-rotating massive elliptical galaxy in the MASSIVE survey. We measure stellar kinematics in 135 spatial bins in the central 1.5 kpc by 2 kpc region of the galaxy using high signal-to-noise (S/N ∼ 130) spectra from the Gemini-North GMOS integral-field spectrograph (IFS). Combining with wide-field IFS kinematics out to ∼ 3 effective radii and stellar light distributions from Hubble Space Telescope (HST ) WFC3 images, we perform Schwarzschild orbit-based mass modeling in the axisymmetric limit to constrain the mass components in NGC 1453. The best-fit black hole mass is M BH = (2.9 ± 0.4) × 10 9 M ; the mass models without a central black hole are excluded at the 8.7σ level. The NGC 1453 black hole lies within the intrinsic scatter of the SMBH and galaxy scaling relations, unlike three other galaxies hosting 10 10 M SMBHs in the MASSIVE sample. The high-S/N GMOS spectra enable us to determine 8 moments of the Gauss-Hermite expansion of the line-of-sight velocity distributions (LOSVDs), which are used as constraints in the orbit modeling. The stellar orbits in the mass models are further constrained to produce negligible h 9 through h 12 to minimize spurious behavior in the LOSVDs. We show that truncating the series at h 4 , as was often done in prior work, leads to a much weaker constraint on the inferred M BH for NGC 1453. Furthermore, we discuss precautions and modifications that are needed to achieve axisymmetry in triaxial orbit codes that use the Schwarzschild method to sample the start space of stellar orbits in triaxial gravitational potentials.

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Section: Photometric Datamentioning

confidence: 99%

The MASSIVE Survey. XV. A Stellar Dynamical Mass Measurement of the Supermassive Black Hole in Massive Elliptical Galaxy NGC 1453

Liepold

Quenneville

et al. 2020

ApJ

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“…Yi et al 2005;Pipino et al 2009;Salim & Rich 2010;Bettoni et al 2014;Davis et al 2015;Haines et al 2015;Stasińska et al 2015;Sheen et al 2016;Vazdekis et al 2016;López-Corredoira & Vazdekis 2018), but also that some post-main-sequence stellar evolutionary phases are also efficient UV emitters (e.g. post-asymptotic giant branch -post-AGB -, blue horizontal branch -HB -stars, binary systems in interaction, and so on, Greggio & Renzini 1990;Brown 1999;O'Connell 1999;Greggio & Renzini 1999;Deharveng et al 2002;Brown 2004;Yoon et al 2004;Maraston 2005;Han et al 2007;Coelho et al 2009;Donahue et al 2010;Loubser & Sánchez-Blázquez 2011;Hernández-Pérez & Bruzual 2014, and references therein).…”

Section: Introductionmentioning

confidence: 99%

UV bright red-sequence galaxies: how do UV upturn systems evolve in redshift and stellar mass?

Dantas

Coelho

Gonçalves

2019

Monthly Notices of the Royal Astronomical Society

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The so-called ultraviolet (UV) upturn of elliptical galaxies is a phenomenon characterised by the up-rise of their fluxes in bluer wavelengths, typically in the 1,200-2,500 A range. This work aims at estimating the rate of occurrence of the UV upturn over the entire red-sequence population of galaxies that show significant UV emission. This assessment is made considering it as function of three parameters: redshift, stellar mass, and -what may seem counter-intuitive at first -emission-line classification. We built a multiwavelength spectro-photometric catalogue from the Galaxy Mass Assembly survey, together with aperture-matched data from Galaxy Evolution Explorer and Sloan Digital Sky Survey, covering the redshift range between 0.06 and 0.40. From this sample, we analyse the UV emission among UV bright galaxies, by selecting those that occupy the red-sequence locus in the (NUV-r) × (FUV-NUV) chart; then, we stratify the sample by their emission-line classes. To that end, we make use of emission-line diagnostic diagrams, focusing the analysis in retired/passive lineless galaxies. Then, a Bayesian logistic model was built to simultaneously deal with the effects of all galaxy properties (including emission-line classification or lack thereof). The main results show that retired/passive systems host an up-rise in the fraction of UV upturn for redshifts between 0.06 and 0.25, followed by an in-fall up to 0.35. Additionally, we show that the fraction of UV upturn hosts rises with increasing stellar mass.

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“…This paper is part of a series of papers investigating an overall sample of 49 BCGs in the nearby Universe for which we have obtained high S/N, long‐slit spectra on the Gemini and William Herschel (WHT) telescopes. The spatially resolved kinematics, central single stellar population (SSP) parameters and the ultraviolet upturn of the BCGs were presented in Loubser et al (, , hereafter Paper 1 and 2, respectively) and Loubser & Sánchez‐Blázquez (). The Mg 2 gradients of a subsample of BCGs with sufficient S/N values were presented in Loubser & Sánchez‐Blázquez (, hereafter Paper 3).…”

Section: Introductionmentioning

confidence: 99%

Stellar population gradients in brightest cluster galaxies

Loubser

Sánchez‐Blázquez

2012

Monthly Notices of the Royal Astronomical Society

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We present the stellar population and velocity dispersion gradients for a sample of 24 brightest cluster galaxies (BCGs) in the nearby Universe for which we have obtained high quality long-slit spectra at the Gemini telescopes. With the aim of studying the possible connection between the formation of the BCGs and their host clusters, we explore the relations between the stellar population gradients and properties of the host clusters as well as the possible connections between the stellar population gradients and other properties of the galaxies. We find mean stellar population gradients (nega-tive ∆[Z/H]/log r gradient of-0.285±0.064; small positive ∆log (age)/log r gradient of 0.069±0.049; and null ∆[E/Fe]/log r gradient of-0.008±0.032) that are consistent with those of normal massive elliptical galaxies. However, we find a trend between metallicity gradients and velocity dispersion (with a negative slope of-1.616±0.539) that is not found for the most massive ellipticals. Furthermore, we find trends between the metallicity gradients and K-band luminosities (with a slope of 0.173±0.081) as well as the distance from the BCG to the X-ray peak of the host cluster (with a slope of-7.546±2.752). The latter indicates a possible relation between the formation of the cluster and that of the central galaxy.

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The ultraviolet upturn in brightest cluster galaxies

Cited by 31 publications

References 73 publications

The MASSIVE Survey. XV. A Stellar Dynamical Mass Measurement of the Supermassive Black Hole in Massive Elliptical Galaxy NGC 1453

The MASSIVE Survey. XV. A Stellar Dynamical Mass Measurement of the Supermassive Black Hole in Massive Elliptical Galaxy NGC 1453

UV bright red-sequence galaxies: how do UV upturn systems evolve in redshift and stellar mass?

Stellar population gradients in brightest cluster galaxies

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