MORE GALAXIES IN THE LOCAL VOLUME IMAGED IN Hα

Караченцев, И. Д.; Кайсин, С. С.

doi:10.1088/0004-6256/140/5/1241

Cited by 38 publications

(43 citation statements)

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“…Similar values were calculated at z ∼ 0 from the SDSS (Brinchmann et al 2004;Nakamura et al 2004) and SINGG (Hanish et al 2006) projects, and from local volume studies (James et al 2008;Karachentsev & Kaisin 2010). Several authors extended local studies to redshifts z < 0.3 using optical spectroscopy (Tresse & Maddox 1998;Sullivan et al 2000).…”

Section: Introductionsupporting

confidence: 65%

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Gómez-Guijarro

Gallego

Villar

et al. 2016

A&A

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Context. Studies measuring the star formation rate density, luminosity function, and properties of star-forming galaxies are numerous. However, it exists a gap at 0.5 < z < 0.8 in Hα-based studies. Aims. Our main goal is to study the properties of a sample of faint Hα emitters at z ∼ 0.62. We focus on their contribution to the faint end of the luminosity function and derived star formation rate density, characterising their morphologies and basic photometric and spectroscopic properties. Methods. We use a narrow-band technique in the near-infrared, with a filter centred at 1.06 µm. The data come from ultra-deep VLT/HAWK-I observations in the GOODS-S field with a total of 31.9 h in the narrow-band filter. In addition to our survey, we mainly make use of ancillary data coming from the CANDELS and Rainbow Cosmological Surveys Database, from the 3D-HST for comparison, and also spectra from the literature. We perform a visual classification of the sample and study their morphologies from structural parameters available in CANDELS. In order to obtain the luminosity function, we apply a traditional V/V max method and perform individual extinction corrections for each object to accurately trace the shape of the function. Results. Our 28 Hα-selected sample of faint star-forming galaxies reveals a robust faint-end slope of the luminosity function α = −1.46 +0.16 −0.08 . The derived star formation rate density at z ∼ 0.62 is ρ SFR = 0.036 +0.012 −0.008 M yr −1 Mpc −3 . The sample is mainly composed of disks, but an important contribution of compact galaxies with Sérsic indexes n ∼ 2 display the highest specific star formation rates. Conclusions. The luminosity function at z ∼ 0.62 from our ultra-deep data points towards a steeper α when an individual extinction correction for each object is applied. Compact galaxies are low-mass, low-luminosity, and starburst-dominated objects with a light profile in an intermediate stage from early to late types.

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Section: Introductionsupporting

confidence: 65%

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Gómez-Guijarro

Gallego

Villar

et al. 2016

A&A

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“…Those cases are suspect, as such behaviour is not found in any of the other surveys. HE04 and Karachentsev & Kaisin (2010) show virtually no SFRs above 0.5 M ⊙ yr −1 , which can be attributed to the fact that their samples are mostly or totally composed of irregular galaxies with very low SFRs.…”

Section: Other Studiesmentioning

confidence: 97%

“…Finally, Karachentsev & Kaisin (2010) presented a study of 52 galaxies observed in Hα as part of a larger survey aimed to study a sample of galaxies in the Local Volume (207 galaxies within 10 Mpc). An important number of the galaxies observed belong to the Maffei 2/IC 342 complex.…”

Section: Ot H E R S T U D I E Smentioning

confidence: 99%

“…Figure 14. Histograms comparing the RC3 Hubble stage distribution, T, of our sample (top left-hand panel) with several samples found in the literature: the Gavazzi et al (2002Gavazzi et al ( , 2006 survey of nearby galaxy clusters, the SINGS sample (Kennicutt et al 2003), the sample of irregular and Sm galaxies observed by Hunter & Elmegreen (2004), HαGS (James et al 2004), the SINGG survey (Meurer et al 2006), the volume-limited sample within 11 Mpc studied by Kennicutt et al (2008) and the 52 galaxies observed in Hα by Karachentsev & Kaisin (2010) as part of a larger Local Volume survey. Note that the last bin in each histogram includes the galaxies with values of T larger than the upper limit in the plot.…”

Section: O N C L U S I O N S a N D F U T U R E W O R Kmentioning

confidence: 99%

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The JCMT Nearby Galaxies Legacy Survey - VII. H imaging and massive star formation properties

Sánchez-Gallego

Knapen

Wilson

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present Hα fluxes, star formation rates (SFRs) and equivalent widths (EWs) for a sample of 156 nearby galaxies observed in the 12CO J= 3–2 line as part of the James Clerk Maxwell Telescope Nearby Galaxies Legacy Survey. These are derived from images and values in the literature and from new Hα images for 72 galaxies which we publish here. We describe the sample, observations and procedures to extract the Hα fluxes and related quantities. We discuss the SFR properties of our sample and confirm the well‐known correlation with galaxy luminosity, albeit with high dispersion. Our SFRs range from 0.1 to 11 M⊙ yr−1 with a median SFR value for the complete sample of 0.2 M⊙ yr−1. This median value is somewhat lower than similar published measurements, which we attribute, in part, to our sample being H i selected and, thus, not biased towards high SFRs as has frequently been the case in previous studies. Additionally, we calculate internal absorptions for the Hα line, A(Hα), which are lower than many of those used in previous studies. Our derived EWs, which range from 1 to 880 Å with a median value of 27 Å, show little dependence on luminosity but rise by a factor of 5 from early‐ to late‐type galaxies. This paper is the first in a series aimed at comparing SFRs obtained from Hα imaging of galaxies with information derived from other tracers of star formation and atomic and molecular gas.

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“…3-3 reproduced from Karachentsev and Kaisin (2010) who combined Hα observations from galaxies within 8 Mpc (in addition, the overplotted open square indicates typical values for the Milky Way). This can be seen in > Fig.…”

Section: Star Formation In the Local Galaxiesmentioning

confidence: 99%

Planets, Stars and Stellar Systems

Oswalt¹,

Keel²

2013

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MORE GALAXIES IN THE LOCAL VOLUME IMAGED IN Hα

Cited by 38 publications

References 84 publications

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

The JCMT Nearby Galaxies Legacy Survey - VII. H imaging and massive star formation properties

Planets, Stars and Stellar Systems

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