The KPNO International Spectroscopic Survey. II. Hα-selected Survey List 1

Salzer, John J.; Grönwall, C.; Lipovetsky, V. A.; Kniazev, A. Y.; Moody, J. W.; Boroson, Todd A.; Thuan, T. X.; Izotov, Y. I.; Herrero, José Luís Caro; Frattare, L. M.

doi:10.1086/318040

Cited by 54 publications

(58 citation statements)

References 23 publications

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“…The design and survey strategy of J-PLUS allows us to probe the faint end of the LF(Hα). It is expected to reach ∼10 38 erg s −1 , which is 2.5 orders of magnitude deeper than the UCM Survey and the KPNO International Spectroscopic Survey (KISS, Salzer et al 2000Salzer et al , 2001. In addition, thanks to the large surveyed volume, the bright end of the luminosity function is also constrained.…”

Section: Introductionmentioning

confidence: 93%

Extracting Hαflux from photometric data in the J-PLUS survey

Vilella-Rojo

Viironen

López-Sanjuan

et al. 2015

A&A

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Aims. We present the main steps that will be taken to extract Hα emission flux from Javalambre Photometric Local Universe Survey (J-PLUS) photometric data.Methods. For galaxies with z 0.015, the Hα+[N ] emission is covered by the J-PLUS narrow-band filter F660. We explore three different methods to extract the Hα + [N ] flux from J-PLUS photometric data: a combination of a broad-band and a narrow-band filter (r and F660), two broad-band and a narrow-band filter (r , i and F660), and an SED-fitting based method using eight photometric points. To test these methodologies, we simulated J-PLUS data from a sample of 7511 SDSS spectra with measured Hα flux. Based on the same sample, we derive two empirical relations to correct the derived Hα+[N ] flux from dust extinction andResults. We find that the only unbiased method is the SED-fitting based method. The combination of two filters underestimates the measurements of the Hα + [N ] flux by 22%, while the three filters method are underestimated by 9%. We study the error budget of the SED-fitting based method and find that, in addition to the photometric error, our measurements have a systematic uncertainty of 4.3%. Several sources contribute to this uncertainty: the differences between our measurement procedure and that used to derive the spectroscopic values, the use of simple stellar populations as templates, and the intrinsic errors of the spectra, which were not taken into account. Apart from that, the empirical corrections for dust extinction and [N ] contamination add an extra uncertainty of 14%. Conclusions. Given the J-PLUS photometric system, the best methodology to extract Hα + [N ] flux is the SED-fitting based method. Using this method, we are able to recover reliable Hα fluxes for thousands of nearby galaxies in a robust and homogeneous way. Moreover, each stage of the process (emission line flux, dust extinction correction, and [N ] decontamination) can be decoupled and improved in the future. This method ensures reliable Hα measurements for many studies of galaxy evolution, from the local star formation rate density, to 2D studies in spatially well-resolved galaxies or the study of environmental effects, up to m r = 21.8 (AB; 3σ detection of Hα+[N ] emission).

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Section: Introductionmentioning

confidence: 93%

Extracting Hαflux from photometric data in the J-PLUS survey

Vilella-Rojo

Viironen

López-Sanjuan

et al. 2015

A&A

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“…In addition to the main fields in the eight clusters we imaged three square-degree strips in the northern periphery of A1656 in order to overlap one of the strips covered by the deeper KISS objective prism survey (Salzer et al 2001). This provided us with a direct comparison of the emission-line galaxy identifications and integrated flux measurements using the imaging and prism techniques.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…The most complete emission-line surveys of the local universe have come from objective prism studies (e.g., Gallego et al 1997;Salzer et al 2001;Moss & Whittle 2000Gronwall et al 2004;Bongiovanni et al 2005;Jangren et al 2005) or multi-fiber surveys such as SDSS and the Two-Degree Field (2dF) survey (e.g., Gómez et al 2003;Hopkins et al 2003;Balogh et al 2004;Brinchmann et al 2004). The prism and fiber spectra have the advantage of uniform coverage over large areas of sky and redshift depth, sufficient to estimate the local cosmological star formation density (e.g., Gallego et al 1995).…”

Section: Introductionmentioning

confidence: 99%

“…One was to achieve a better understanding of the observational selection effects in SFR surveys that was alluded to earlier. The eight clusters have been studied independently in an objective prism survey by Moss & Whittle (2000), and by comparing our own image-based inventory of galaxies and SFRs with their measurements (and overlapping regions in one of the clusters by the Kitt Peak International Spectroscopic Survey (KISS; Salzer et al 2001)), we can obtain at least an approximate measurement of the incompleteness in the prism- based SFRs and cosmic SFR densities. We can also use the data to simulate fiber or slit-based spectroscopic measurements for arbitrary aperture sizes and galaxy redshifts, and in this way assess the importance of aperture effects in characterizing the SFRs of present-day cluster members.…”

Section: Introductionmentioning

confidence: 99%

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A DEEP, WIDE-FIELD Hα SURVEY OF NEARBY CLUSTERS OF GALAXIES: DATA

Sakai

Kennicutt

Moss

2012

ApJS

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We present the results of a wide-field Hα imaging survey of eight nearby (z = 0.02-0.03) Abell clusters. We have measured Hα fluxes and equivalent widths for 465 galaxies, of which 360 are new detections. The survey was designed to obtain complete emission-line-selected inventories of star-forming galaxies in the inner regions of these clusters, extending to star formation rates below 0.1 M yr −1 . This paper describes the observations, data processing, and source identification procedures, and presents an Hα and R-band catalog of detected cluster members and other candidates. Future papers in the series will use these data to study the completeness of spectroscopically based star formation surveys, and to quantify the effects of cluster environment on the present-day populations of star-forming galaxies. The data will also provide a valuable foundation for imaging surveys of redshifted Hα emission in more distant clusters.

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“…The survey is thus a unique resource for probing the nature of star-forming and active galaxies 3 in the nearby universe. A full description of the survey can be found in Salzer et al (2000Salzer et al ( , 2001.…”

Section: The Kpno International Spectroscopic Surveymentioning

confidence: 99%

Objective-Prism Emission-Line Searches for Active Galactic Nuclei

Grönwall

Sarajedini

Salzer

2002

International Astronomical Union Colloquium

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Abstract. Objective-prism surveys for UV-excess and emission-line objects, especially the First and Second Byurakan Surveys, have been central to the study of active galactic nuclei (AGNs). We review previous line-selected surveys for AGNs and discuss their contribution to our understanding of the AGN phenomena. In addition, we present results from the KPNO International Spectroscopic Survey, a modern digital objective-prism survey for emission line objects. This survey is discovering substantial numbers of new AGNs, in particular low-luminosity AGNs and LINERs.

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The KPNO International Spectroscopic Survey. II. Hα-selected Survey List 1

Cited by 54 publications

References 23 publications

Extracting Hαflux from photometric data in the J-PLUS survey

Extracting Hαflux from photometric data in the J-PLUS survey

A DEEP, WIDE-FIELD Hα SURVEY OF NEARBY CLUSTERS OF GALAXIES: DATA

Objective-Prism Emission-Line Searches for Active Galactic Nuclei

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