The Balmer decrement of Sloan Digital Sky Survey galaxies

Groves, Brent; Brinchmann, Jarle; Walcher, C. J.

doi:10.1111/j.1365-2966.2011.19796.x

Cited by 108 publications

(114 citation statements)

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“…The attenuation based on Hδ/Hβ is lower at bright magnitudes, high masses, and low star formation rates. Such an offset is also reported by Groves et al (2012) based on measurements from the SDSS DR7 data set and is thought to be caused by a systematic error in the continuum fit around the Hδ line. The exact source of the discrepancy, however, is still being investigated by the SDSS collaboration (J. Brinchmann 2011, private communication).…”

Section: Nebular Dust Attenuation In a Comparison Sample Of Local Galsupporting

confidence: 65%

NEBULAR ATTENUATION IN Hα-SELECTED STAR-FORMING GALAXIES ATz= 0.8 FROM THE NewHα SURVEY

Momcheva

Lee

et al. 2013

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We present measurements of the dust attenuation of Hα-selected emission-line galaxies at z = 0.8 from the NewHα narrowband survey. The analysis is based on deep follow-up spectroscopy with Magellan/IMACS, which captures the strong rest-frame optical emission lines fromThe spectroscopic sample used in this analysis consists of 341 confirmed Hα emitters. We place constraints on the active galactic nucleus (AGN) fraction using diagnostics that can be applied at intermediate redshift. We find that at least 5% of the objects in our spectroscopic sample can be classified as AGNs and 2% are composite, i.e., powered by a combination of star formation and AGN activity. We measure the dust attenuation for individual objects from the ratios of the higher order Balmer lines. The Hβ and Hγ pair of lines is detected with S/N > 5 in 55 individual objects and the Hβ and Hδ pair is detected in 50 individual objects. We also create stacked spectra to probe the attenuation in objects without individual detections. The median attenuation at Hα based on the objects with individually detected lines is A(Hα) = 0.9 ± 1.0 mag, in good agreement with the attenuation found in local samples of star-forming galaxies. We find that the z = 0.8 galaxies occupy a similar locus of attenuation as a function of magnitude, mass, and star formation rate (SFR) as a comparison sample drawn from the SDSS DR4. Both the results from the individual z = 0.8 galaxies and from the stacked spectra show consistency with the mass-attenuation and SFR-attenuation relations found in the local universe, indicating that these relations are also applicable at intermediate redshift.

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Section: Nebular Dust Attenuation In a Comparison Sample Of Local Galsupporting

confidence: 65%

NEBULAR ATTENUATION IN Hα-SELECTED STAR-FORMING GALAXIES ATz= 0.8 FROM THE NewHα SURVEY

Momcheva

Lee

et al. 2013

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“…The Hα/Hβ ratio (Balmer decrement), sensitive to dust extinction, is measured as 5.00, high compared to 2.86 expected for dust-free star-forming galaxies. The intrinsic ratio may be slightly higher for AGN e.g ∼ 3.1 assumed by Groves, Brinchmann and Walcher (2012), while our bestfit model described below predicts 2.95. Even for the highest of these values, on the basis of the Calzetti extinction law (Calzetti et al 2000) the extinction is a factor of (5.0/3.1) 2.615 = 3.49 in Hα, or a reddening E(B−V) = 0.408 mag.…”

Section: Extracting the Spectramentioning

confidence: 57%

MUSE three-dimensional spectroscopy and kinematics of the gigahertz peaked spectrum radio galaxy PKS 1934–63: interaction, recently triggered active galactic nucleus and star formation

Roche

Humphrey

Lagos

et al. 2016

Mon. Not. R. Astron. Soc.

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We observe the radio galaxy PKS 1934-63 (at z = 0.1825) using MUSE (Multi Unit Spectroscopic Explorer) on the Very Large Telescope (VLT). The radio source is GigaHertz Peaked Spectrum and compact (0.13 kpc), implying an early stage of evolution (≤ 10 4 yr). Our data show an interacting pair of galaxies, projected separation 9.1 kpc, velocity difference ∆(v) = 216 km s −1 . The larger galaxy is a M * 10 11 M spheroidal with the emission-line spectrum of a high-excitation young radio AGN, e.g. strong [OI]6300 and [OIII]5007. Emission-line ratios indicate a large contribution to the line luminosity from high-velocity shocks ( 550 km s −1 ) . The companion is a non-AGN disk galaxy, with extended Hα emission from which its star-formation rate is estimated as 0.61 M yr −1 . Both galaxies show rotational velocity gradients in Hα and other lines, with the interaction being prograde-prograde. The SE-NW velocity gradient of the AGN host is misaligned from the E-W radio axis, but aligned with a previously discovered central ultraviolet source, and a factor 2 greater in amplitude in Hα than in other (forbidden) lines (e.g. [OIII]5007). This could be produced by a fast rotating (100-150 km s −1 ) disk with circumnuclear star-formation. We also identify a broad component of [OIII]5007 emission, blueshifted with a velocity gradient aligned with the radio jets, and associated with outflow. However, the broad component of [OI]6300 is redshifted. In spectral fits, both galaxies have old stellar populations plus ∼ 0.1% of very young stars, consistent with the galaxies undergoing first perigalacticon, triggering infall and star-formation from ∼ 40 Myr ago followed by the radio outburst.

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“…The SSP grid spans three metallicities (Z = 0.004, 0.02, and 0.05), 15 formation ages ranging from 10 Myr to 13 Gyr, and assumes a Chabrier initial mass function (Chabrier 2003) along with the Cardelli et al (1989) extinction law (R v = 3.1). We chose to use the models of Bruzual & Charlot (2003) instead of Charlot & Bruzual (2007;unpublished, updated of Bruzual & Charlot 2003) because although the newer models incorporate a better treatment of the thermally pulsating asymptotic giant branch (TP-AGB) stars, they lead to an underestimation of the stellar continuum around the Hβ line (Groves et al 2012).…”

Section: Methodsmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): Improved emission lines measurements in four representative samples at 0.07 <z< 0.3

Rodrigues

Foster

Taylor

et al. 2016

A&A

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This paper presents a new catalog of emission lines based on the GAMA II data for galaxies between 0.07 < z < 0.34. The catalog includes four subsamples containing 3000 galaxies drawn from the GAMA II survey and spanning four redshift windows. The four samples are representative of intermediate-mass galaxies down to log M * > 9.4 at z ∼ 0.1 and log M * > 10.6 at z ∼ 0.30. We have developed a dedicated code called MARVIN that automates the main steps of the data analysis, but imposes visual individual quality control of each measurement. We use this catalog to investigate how the sample selection influences the shape of the stellar massmetallicity relation. We find that commonly used selection criteria on line detections and by AGN rejection could affect the shape and dispersion of the high-mass end of the M − Z relation. For log M * > 10.6, common selection criteria reject about 65% of the emission-line galaxies. We also find that the relation does not evolve significantly from z = 0.07 to z = 0.34 in the range of stellar mass for which the samples are representative (log M * > 10.6). For lower stellar masses (log M * < 10.2) we are able to show that the observed 0.15 dex metallicity decrease in the same redshift range is a consequence of a color bias arising from selecting targets in the r-band. We highlight that this color selection bias affects all samples selected in r-band (e.g., GAMA and SDSS), even those drawn from volume-limited samples. Previously reported evolution of the M − Z relation at various redshifts may need to be revised to evaluate the effect of this selection bias.

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The Balmer decrement of Sloan Digital Sky Survey galaxies

Cited by 108 publications

References 50 publications

NEBULAR ATTENUATION IN Hα-SELECTED STAR-FORMING GALAXIES ATz= 0.8 FROM THE NewHα SURVEY

NEBULAR ATTENUATION IN Hα-SELECTED STAR-FORMING GALAXIES ATz= 0.8 FROM THE NewHα SURVEY

MUSE three-dimensional spectroscopy and kinematics of the gigahertz peaked spectrum radio galaxy PKS 1934–63: interaction, recently triggered active galactic nucleus and star formation

Galaxy And Mass Assembly (GAMA): Improved emission lines measurements in four representative samples at 0.07 <z< 0.3

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