An Hα Imaging Survey of Galaxies in the Local 11 Mpc Volume

By Robert C. Kennicutt Jr., Janice C. Lee, J. Funes, S. J., S. Sakai, Sanae Akiyama. 2004

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As part of a broader effort to characterize the population of star-forming galaxies in the local universe, we have carried out an H α + [N II] imaging survey for an essentially volume-limited sample of galaxies within 11 Mpc of the Milky Way. This first paper describes the design of the survey, the observation, data processing, and calibration procedures, and the characteristics of the galaxy sample. The main product of the paper is a catalog of integrated Hα fluxes, luminosities, and equivalent widths for the galaxies in the sample. We briefly discuss the completeness properties of the survey and compare the distribution of the sample and its star formation properties to other large Hα imaging surveys. These data form the foundation for a series of follow-up studies of the star formation properties of the local volume, and the properties and duty cycles of star formation bursts in dwarf galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/09b50c07d6b2572151e8d3426b86f829b3716cd7

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Citations in the corpus

The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types (2014, background): “Total Hα fluxes are taken from Gil de Paz et al. (2003); Moustakas & Kennicutt (2006); Kennicutt et al. (2008); Östlin et al. (2009).”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS (2009, methodology): “For an additional 13 galaxies, we applied the mean relation between average [N ii]/Hα and MB in the MK06 sample, as published in Kennicutt et al. (2008).”
Probing the role of the galactic environment in the formation of stellar clusters, using M83 as a test bench (2015, methodology): “We calibrated the total luminosity estimated from this frame (after masking residuals at the location of foreground stars) to the total Hα luminosity published by Kennicutt et al. (2008), giving us a correction factor that takes into account [Nii] contamination and foreground galactic extinction.”
A MOLECULAR STAR FORMATION LAW IN THE ATOMIC-GAS-DOMINATED REGIME IN NEARBY GALAXIES (2011, methodology): “For the literature and several problematic SINGS targets, we pin the total Hα+[N ii] flux to published values, usually those of Kennicutt et al. (2008).”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, methodology): “The SFR within 11 Mpc has been measured by the 11 Mpc Hα and Ultraviolet Galaxy Survey (11HUGS; Kennicutt et al. 2008; Bothwell et al. 2011).”
A GALEX ULTRAVIOLET IMAGING SURVEY OF GALAXIES IN THE LOCAL VOLUME (2010, methodology): “Together with the precursor Hα survey and the Local Volume Legacy infrared observations with Spitzer (as described in Kennicutt et al. 2008 and Dale et al. 2009 respectively), the GALEX observations reported here furnish a core dataset for studying star formation and dust in the Galactic…”
DWARF GALAXY STARBURST STATISTICS IN THE LOCAL VOLUME (2008, methodology): “Here, we use data from the completed Hα component of the parent survey (Kennicutt et al. 2008), which provides tracers of the SFRs and birthrates (ratio of the present to past average SFR) over the past few million years, to calculate the dwarf galaxy starburst statistics described above.”
THE SPITZER LOCAL VOLUME LEGACY: SURVEY DESCRIPTION AND INFRARED PHOTOMETRY (2009, methodology): “The outer tier of LVL is derived from the larger 11 Mpc narrowband Hα imaging survey of Kennicutt et al. (2008), and GALEX ultraviolet follow-up observations of a subsample which avoids the Galactic plane (|b| > 30◦) (Lee et al. 2009a).”
THE CALIBRATION OF MONOCHROMATIC FAR-INFRARED STAR FORMATION RATE INDICATORS (2010, methodology): “In the LVL and SINGS samples we retain four galaxies, M81DwA, HolmbergIX, UGC6900, and UGC9128, which are undetected or marginally detected in the MIPS bands, but have Hα measurements; these galaxies are metal poor, and consequently, dust–poor, thus likely to have most of their star formation light ”
THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, methodology): “There were 13 additional galaxies for which we did not have Hα fluxes but which were included in Kennicutt et al. (2008), and we used their fluxes for these galaxies, which are marked in Table 1 (with the superscript e).”
COMPARISON OF Hα AND UV STAR FORMATION RATES IN THE LOCAL VOLUME: SYSTEMATIC DISCREPANCIES FOR DWARF GALAXIES (2009, methodology): “In order to further study the relationship between the UV and Hα emission, we draw upon GALEX UV observations for a complete sub-set of star-forming galaxies from the 11 Mpc Hα narrowband imaging survey of Kennicutt et al. (2008).”
THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I. HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS (2014, background): “Most constraints on star formation efficiency for low mass galaxies come from studies of recent star formation (e.g., Hα, UV, 24 µm) and current gas content (e.g., Leroy et al. 2008; Salim et al. 2007; Kennicutt et al. 2008; Lee et al. 2011; Kennicutt & Evans 2012).”
Fitting the integrated spectral energy distributions of galaxies (2010, background): “LVL consolidates and builds upon recent Local Volume galaxy surveys which have acquired groundbased narrowband Hα (Kennicutt et al. 2008), GALEX ultraviolet (Lee et al., in prep.) and HST resolved stellar population imaging (Dalcanton et al. 2009), by collecting Spitzer IRAC and MIPS infrared…”
TOWARD A UNIFICATION OF STAR FORMATION RATE DETERMINATIONS IN THE MILKY WAY AND OTHER GALAXIES (2011, methodology): “4, we plot the product of their measured point-source luminosities and YXP fractions, rescaled to the distances listed in Kennicutt et al. (2008) and Moustakas & Kennicutt (2006).”
UPDATED NEARBY GALAXY CATALOG (2013, methodology): “The main source of the flux data is the Hα-survey of the LV galaxies performed at the 6-m BTA telescope of SAO RAS (Kaisin & Karachentsev 2006, 2008; Karachentsev & Kaisin 2007, 2010), as well as the survey by Kennicutt et al. (2008).”
DIRECT OXYGEN ABUNDANCES FOR LOW-LUMINOSITY LVL GALAXIES (2012, methodology): “The LVL is leveraged by ancillary data including Hα (Kennicutt et al. 2008) and UV (Lee et al. 2011) imaging from the 11 Mpc Hα and Ultraviolet Galaxy Survey (11HUGS; Lee et al. 2011) and the Nearby Galaxy Survey (NGS; Gil de Paz et al. 2007).”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “…(ideally volume-limited) selection criteria, and studies of this kind (based on UV, visible, and/or Hα observations) have been carried out by several groups (e.g., Karachentsev et al. 2004; Blanton et al. 2005; Meurer et al. 2006; Kennicutt et al. 2008; Dalcanton et al. 2009; Hunter et al. 2010).”