The KPNO International Spectroscopic Survey. I. Description of the Survey

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:10.1086/301418

Cited by 98 publications

(124 citation statements)

References 43 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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“…Apart from the obvious importance of measuring a physical quantity in two independent ways, there are at least two additional incentives to comparing UV and Balmer line luminosities. First, many of the surveys at lower redshifts have been based on Ha (e.g., Gallego et al 1995 ;Salzer et al 2000 ;Tresse & Maddox 1998 ;Glazebrook et al 1999 ;Yan et al 1999 ;Moorwood et al 2000) ; clearly, it is desirable to use the same measure (or two closely related ones such as Ha and Hb) when considering the evolution with redshift of global properties such as the volume-averaged SFR density. Second, almost by deÐnition, all interstellar reddening curves rise from the optical to the UV.…”

Section: Star Formation Rates and Dust Extinctionmentioning

confidence: 99%

The Rest‐Frame Optical Spectra of Lyman Break Galaxies: Star Formation, Extinction, Abundances, and Kinematics

Pettini

Shapley

Steidel

et al. 2001

ApJ

740

972

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We present the Ðrst results of a spectroscopic survey of Lyman break galaxies (LBGs) in the nearinfrared aimed at detecting the emission lines of [O II], [O III], and Hb from the H II regions of normal star-forming galaxies at z^3. From observations of 15 objects with the Keck telescope and the Very Large Telescope augmented with data from the literature for an additional four objects, we reach the following main conclusions. The rest-frame optical properties of LBGs at the bright end of the luminosity function are remarkably uniform, their spectra are dominated by emission lines, [O III] is always stronger than Hb and [O II], and projected velocity dispersions are between 50 and 115 km s~1. Contrary to expectations, the star formation rates deduced from the Hb luminosity are on average no larger than those implied by the stellar continuum at 1500 presumably any di †erential extinction between A ; rest-frame optical and UV wavelengths is small compared to the relative uncertainties in the calibrations of these two star formation tracers. For the galaxies in our sample, the abundance of oxygen can only be determined to within 1 order of magnitude without recourse to other emission lines ([N II] and Ha), which are generally not available. Even so, it seems well established that LBGs are the most metalenriched structures at z^3, apart from quasi-stellar objects, with abundances greater than about 1/10 solar and generally higher than those of damped Lya systems at the same epoch. They are also signiÐ-cantly overluminous for their metallicities ; this is probably an indication that their mass-to-light ratios are low compared to present-day galaxies. At face value, the measured velocity dispersions imply virial masses of about 1010 within half-light radii of 2.5 kpc. The corresponding mass-to-light ratios, M _ M/L B 0.15 in solar units, are indicative of stellar populations with ages between 108 and 109 yr, consistent with the UV-optical spectral energy distributions. However, we are unable to establish conclusively whether or not the widths of the emission lines reÑect the motions of the H II regions within the gravitational potential of the galaxies, even though in two cases we see hints of rotation curves. All 19 LBGs observed show evidence for galactic-scale superwinds ; such outÑows have important consequences for regulating star formation, distributing metals over large volumes, and allowing Lyman continuum photons to escape and ionize the intergalactic medium.

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“…The reddening was determined using the reddening law of Cardelli et al (1989) The black points are from the SHIELD galaxies in this work, those with outer circles are H ii regions for which we obtained a measurement of the temperature sensitive [O iii] λ4363 line. The green triangles are galaxies from the ADBS survey ) and the gray points are a large sample of emission line sources from the KISS survey (e.g., Salzer et al 2000;Melbourne & Salzer 2002). The solid line traces the star-forming galaxy models of Dopita & Evans (1986); the dashed line (Kauffmann et al 2003) delineates the region of the diagram usually occupied by AGNs.…”

Section: Spectral Reduction and Measurementmentioning

confidence: 99%

“…SHIELD galaxies are plotted on Figure 3 as solid black points; those with circles around them are the two H ii regions that displayed a measurable [O iii] λ4363 flux. The green triangles represent H ii regions in low H i mass dIrr galaxies from the ADBS, which is a similarly selected, but more luminous, sample , and the gray points are galaxies from the KPNO International Spectroscopic Survey (KISS; e.g., Salzer et al 2000;Melbourne & Salzer 2002;Salzer et al 2005a). The dashed line differentiates active galactic nuclei (AGNs) from star-forming nebulae (Kauffmann et al 2003) and the solid line represents the locus of high excitation starforming nebulae from the models of Dopita & Evans (1986), which increase smoothly in metallicity from the upper left to the lower right.…”

Section: Abundance Determinationmentioning

confidence: 99%

Oxygen Abundance Measurements of Shield Galaxies

Haurberg

Salzer

Cannon

et al. 2015

ApJ

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We have derived oxygen abundances for eight galaxies from the Survey for H i in Extremely Low-mass Dwarfs (SHIELD). The SHIELD survey is an ongoing study of very-low-mass galaxies, with M H i between 10 6.5 and 10 7.5 M , that were detected by the Arecibo Legacy Fast ALFA survey. Hα images from the WIYN 3.5 m telescope show that these eight SHIELD galaxies each possess one or two active star-forming regions, which were targeted with long-slit spectral observations using the Mayall 4 m telescope at Kitt Peak National Observatory. We obtained a direct measurement of the electron temperature by detection of the weak [O iii] λ4363 line in two of the H ii regions. Oxygen abundances for the other H ii regions were estimated using a strong-line method. When the SHIELD galaxies are plotted on a B-band L-Z diagram, they appear to suggest a slightly shallower slope to the relationship than normally seen. However, that offset is systematically reduced when the near-infrared luminosity is used instead. This indicates a different mass-to-light ratio for the galaxies in this sample and we suggest that this may be indicative of differing star formation histories in the lowest luminosity and surface brightness dwarf irregulars.

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The KPNO International Spectroscopic Survey. I. Description of the Survey

Cited by 98 publications

References 43 publications

Extracting Hαflux from photometric data in the J-PLUS survey

Extracting Hαflux from photometric data in the J-PLUS survey

The Rest‐Frame Optical Spectra of Lyman Break Galaxies: Star Formation, Extinction, Abundances, and Kinematics

Oxygen Abundance Measurements of Shield Galaxies

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