KPNO International Spectroscopic Survey Research Articles

Metal Abundances of Intermediate-redshift Active Galactic Nuclei: Evidence for a Population of Lower-metallicity Seyfert 2 Galaxies at z = 0.3–0.4

We derive oxygen abundances for two samples of Seyfert 2 (Sy2) active galactic nuclei (AGNs) selected from the KPNO International Spectroscopic Survey (KISS). The two samples from KISS include 17 intermediate-redshift (0.29 ≤ z ≤ 0.42) Sy2s detected via their [O iii] lines, and 35 low-redshift (z ≤ 0.1), Hα-detected Sy2s. The primary goal of this work is to explore whether the metallicity distribution of these two samples changes with redshift. To determine the oxygen abundances of the KISS galaxies, we use Cloudy to create a large number of photoionization model grids by varying the temperature of the accretion disk, the ratio of X-ray to UV continuum light, the ionization parameter, the hydrogen density, and the metallicity of the narrow-line region clouds. We link the results of these models to the observed [O iii]/Hβ and [N ii]/Hα emission-line ratios of the KISS sample on a Baldwin–Philips–Terlevich diagram, interpolating across the model grids to derive metallicity. The two redshift samples overlap substantially in terms of derived metal abundances, but we find that some of the intermediate-redshift Sy2s possess lower abundances than their local universe counterparts. Our analysis provides evidence for modest levels of chemical evolution (0.18 ± 0.06 dex) over 3–4 Gyr of look-back time. We compare our results to other AGN abundance derivation methods from the literature.

The Environments of Green Pea Galaxies. I. The KISS Sample

Abstract We present environmental analyses for 13 KPNO International Spectroscopic Survey Green Pea (GP) galaxies. These galaxies were discovered via their strong [O iii] emission in the redshift range 0.29 < z < 0.42, and they are undergoing a major burst of star formation. A primary goal of this study is to understand what role the environment plays in driving the current star formation activity. By studying the environments around these extreme star-forming galaxies, we can learn more about what triggers their star formation processes and how they fit into the narrative of galaxy evolution. Using the Hydra multifiber spectrograph on the WIYN 3.5 m telescope, we mapped out the galaxy distribution around each of the GPs (out to ∼15 Mpc at the redshifts of the targets). Using three density analysis methodologies chosen for their compatibility with the geometry of our redshift survey, we categorized the galaxian densities of the GPs into different density regimes. We find that the GPs in our sample tend to be located in low-density environments. We find no correlation between the density and the SFRs seen in the GPs. We conclude that the environments the GPs are found in are likely not the driving factor behind their extreme star formation activity.

Properties of the KISS Green Pea Galaxies

Abstract Green peas (GPs) are a class of extreme star-forming galaxies (SFGs) at intermediate redshifts, originally discovered via color selection using multifilter, wide-field survey imaging data. They are commonly thought of as being analogs of high-redshift Lyα-emitting galaxies. The defining characteristic of GP galaxies is a high-excitation nebular spectrum with very large equivalent width lines, leading to the recognition that GP-like galaxies can also be identified in samples of emission-line galaxies. Here we compare the properties a sample of [O iii]-selected SFGs (z = 0.29–0.41) from the KPNO International Spectroscopic Survey (KISS) with the color-selected GPs. We find that the KISS [O iii]-selected galaxies overlap with the parameter space defined by the color-selected GPs; the two samples appear to be drawn from the same population of objects. We compare the KISS GPs with the full Hα-selected KISS SFG sample (z < 0.1) and find that they are extreme systems. Many appear to be young systems at their observed look-back times (3–4 Gyr), with more than 90% of their rest-frame B-band luminosity coming from the starburst population. We compute the volume density of the KISS red (KISSR) GPs at z = 0.29–0.41 and find that they are extremely rare objects. We do not see galaxies as extreme as the KISSR GPs in the local universe, although we recognize several lower-luminosity systems at z < 0.1.

Metal Abundances and Star Formation Rates of Emission-line Galaxies in and around the Boötes Void

Abstract We explore the possible dependencies of galaxy metal abundance and star formation rate (SFR) on local environment, focusing on the volume of space in and around the Boötes Void. Our sample of star-forming galaxies comes from the second catalog of the Hα-selected KPNO International Spectroscopic Survey (KISS), which overlaps the void. This sample represents a statistically complete, line-flux-limited ensemble of 820 star-forming galaxies, all of which possess metallicity and SFR estimates. We carry out two distinct analyses of the KISS galaxies: one that probes the properties of the entire sample as a function of local density, and a second that details the properties of 33 KISS star-forming galaxies located within the Boötes Void. In both cases, we find no evidence that either the metallicity of the KISS galaxies or their SFRs depend on the environments within which the galaxies are located. Our global analysis does show weak trends for decreasing stellar mass, decreasing metallicity, and decreasing SFRs with decreasing local densities. However, we argue that the metallicity and SFR trends are artifacts of the stellar mass—local density trend. In particular, the change in metallicity with density is precisely what one would predict from the mass–metallicity relation, given the observed drop in stellar mass with decreasing metallicity. Likewise, the SFR trend with density disappears when one instead considers the mass-normalized specific SFR. The KISS galaxies dwelling in the Boötes Void are found to have metallicity and SFR properties nearly identical to those of a matched comparison sample, despite the fact that the former are located in density environments that are, on average, more than 16 times lower.

Metal Abundances of KISS Galaxies. VI. New Metallicity Relations for the KISS Sample of Star-forming Galaxies

Abstract We present updated metallicity relations for the spectral database of star-forming galaxies (SFGs) found in the KPNO International Spectroscopic Survey (KISS). New spectral observations of emission-line galaxies obtained from a variety of telescope facilities provide oxygen abundance information. A nearly fourfold increase in the number of KISS objects with robust metallicities relative to our previous analysis provides for an empirical abundance calibration to compute self-consistent metallicity estimates for all SFGs in the sample with adequate spectral data. In addition, a sophisticated spectral energy distribution fitting routine has provided robust calculations of stellar mass. With these new and/or improved galaxy characteristics, we have developed luminosity–metallicity (L–Z) relations, mass–metallicity (M *–Z) relations, and the so-called fundamental metallicity relation (FMR) for over 1450 galaxies from the KISS sample. This KISS M *–Z relation is presented for the first time and demonstrates markedly lower scatter than the KISS L–Z relation. We find that our relations agree reasonably well with previous publications, modulo modest offsets due to differences in the strong emission line metallicity calibrations used. We illustrate an important bias present in previous L–Z and M *–Z studies involving direct-method (T e ) abundances that may result in systematically lower slopes in these relations. Our KISS FMR shows consistency with those found in the literature, albeit with a larger scatter. This is likely a consequence of the KISS sample being biased toward galaxies with high levels of activity.

METAL ABUNDANCES OF KISS GALAXIES. V. NEBULAR ABUNDANCES OF 15 INTERMEDIATE LUMINOSITY STAR-FORMING GALAXIES

We present high S/N spectroscopy of 15 emission-line galaxies (ELGs) cataloged in the KPNO International Spectroscopic Survey (KISS), selected for their possession of high equivalent width [O III] lines. The primary goal of this study was to attempt to derive direct-method ($T_e$) abundances for use in constraining the upper-metallicity branch of the $R_{23}$ relation. The spectra cover the full optical region from [O II]{\lambda}{\lambda}3726,3729 to [S III]{\lambda}{\lambda}9069,9531 and include the measurement of [O III]{\lambda}4363 in 13 objects. From these spectra, we determine abundance ratios of helium, nitrogen, oxygen, neon, sulfur, and argon. We find these galaxies to predominantly possess oxygen abundances in the range of 8.0 $\lesssim$ 12+log(O/H) $\lesssim$ 8.3. We present a comparison of direct-method abundances with empirical SEL techniques, revealing several discrepancies. We also present a comparison of direct-method oxygen abundance calculations using electron temperatures determined from emission lines of O$^{++}$ and S$^{++}$, finding a small systematic shift to lower $T_e$ (~1184 K) and higher metallicity (~0.14 dex) for sulfur-derived $T_e$ compared to oxygen-derived $T_e$. Finally, we explore in some detail the different spectral activity types of targets in our sample, including regular star-forming galaxies, those with suspected AGN contamination, and a local pair of low-metallicity, high-luminosity compact objects.

Comparing infrared star formation rate indicators with optically derived quantities

We examine the UV reprocessing efficiencies of warm dust and polycyclic aromatic hydrocarbons (PAHs) through an analysis of the mid- and far-infrared surface luminosity densities of 85 nearby H$\alpha$-selected star-forming galaxies detected by the volume-limited KPNO International Spectroscopic Survey (KISS). Because H$\alpha$ selection is not biased toward continuum-bright objects, the KISS sample spans a wide range in stellar masses ($10^8$-$10^{12}\rm{M}_\odot$), as well as H$\alpha$ luminosity ($10^{39}$-$10^{43}\rm{ergs/s}$), mid-infrared 8.0$\mu$m luminosity ($10^{41}$-$10^{44}\rm{ergs/s}$), and [Bw-R] color (-.1-2.2). We find that mid-infrared polycyclic aromatic hydrocarbon (PAH) emission in the Spitzer IRAC 8.0$\mu$m band correlates with star formation, and that the efficiency with which galaxies reprocess UV energy into PAH emission depends on metallicity. We also find that the relationship between far-infrared luminosity in the Spitzer MIPS 24$\mu$m band pass and H$\alpha$-measured star-formation rate varies from galaxy to galaxy within our sample; we do not observe a metallicity dependence in this relationship. We use optical colors and established mass-to-light relationships to determine stellar masses for the KISS galaxies; we compare these masses to those of nearby galaxies as a confirmation that the volume-limited nature of KISS avoids strong biases. We also examine the relationship between IRAC 3.6$\mu$m luminosity and galaxy stellar mass, and find a color-dependent correlation between the two.

A POPULATION OF METAL-POOR GALAXIES WITH ∼L* LUMINOSITIES AT INTERMEDIATE REDSHIFTS

We present new spectroscopy and metallicity estimates for a sample of 15 star-forming galaxies with redshifts in the range 0.29-0.42. These objects were selected in the KPNO International Spectroscopic Survey via their strong emission lines seen in red objective-prism spectra. Originally thought to be intermediate-redshift Seyfert 2 galaxies, our new spectroscopy in the far red has revealed these objects to be metal-poor star-forming galaxies. These galaxies follow a luminosity-metallicity (L – Z) relation that parallels the one defined by low-redshift galaxies, but is offset by a factor of more than 10 to lower abundances. The amount of chemical and/or luminosity evolution required to place these galaxies on the local L–Z relation is extreme, suggesting that these galaxies are in a very special stage of their evolution. They may be late-forming massive systems, which would challenge the current paradigm of galaxy formation. Alternatively, they may represent intense starbursts in dwarf-dwarf mergers or a major infall episode of pristine gas into a pre-existing galaxy. In any case, these objects represent an extreme stage of galaxy evolution taking place at relatively low redshift.

The host galaxy of GRB 031203: a new spectroscopic study

Aims. The host galaxy of the long-duration gamma-ray burst (GRB) 031203 (HG 031203) offers a precious opportunity to study in detail the environment of a nearby GRB. The aim is to better characterize this galaxy and analyse the possible evolution with time of the spectroscopic quantities we derive. Methods. We analyse HG 031203 using a set of optical spectra acquired with the ESO-VLT and Keck telescope. We compare the metallicity, luminosity and star formation properties of this galaxy and of the other supernova-long gamma-ray burst hosts in the local universe (z < 0.2) against the KPNO International Spectroscopic Survey. Results. HG031203 is a metal poor, actively star forming galaxy (star formation rate of 12.9 ± 2.2 M ⊙ yr -1 ) at z = 0.1054. From the emission-line analysis we derive an intrinsic reddening E HG (B - V) ≈ 0.4. This parameter doesn't show a compelling evidence of evolution at a month time-scale. We find an interstellar medium temperature of ≈12 500 K and an electronic density of N e = 160 cm -3 . After investigating for possible Wolf-Rayet emission features in our spectra, we consider dubious the classification of HG 031203 as a Wolf-Rayet galaxy. Long gamma-ray burst (LGRB) and supernova hosts in the local universe (z < 0.2) show, on average, specific star formation rates higher than ordinary star forming galaxy at the same redshift. On the other hand, we find that half of the hosts follows the metallicity-luminosity relation found for star-burst galaxies; HG 031203 is a clear outlier, with its really low metallicity (12 + log (O/H)= 8.12 ± 0.04).

The Diverse Infrared Properties of a Complete Sample of Star‐forming Dwarf Galaxies

We present mid-infrared Spitzer Space Telescope observations of a complete sample of star-forming dwarf galaxies selected from the KPNO International Spectroscopic Survey. The galaxies span a wide range in mid-infrared properties. Contrary to expectations, some of the galaxies emit strongly at 8 μm, indicating the presence of hot dust and/or PAHs. The ratio of this mid-infrared dust emission to the stellar emission is compared with the galaxies' luminosity, star formation rate, metallicity, and optical reddening. We find that the ratio of the 8.0 μm dust emission to the stellar emission is more strongly correlated with the star formation rate than it is with the metallicity or the optical reddening in these systems. Nonetheless, there is a correlation between the 8.0 μm luminosity and metallicity. The slope of this luminosity-metallicity correlation is shallower than corresponding ones in the B band and 3.6 μm. The precise nature of the 8.0 μm emission seen in these galaxies (i.e., PAH vs. hot dust or some combination of the two) will require future study, including deep mid-IR spectroscopy.

The KPNO International Spectroscopic Survey. V. Hα-selected Survey List 3

The KPNO International Spectroscopic Survey (KISS) is an objective-prism survey designed to detect extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies (ELGs). Here we present the third list of ELG candidates selected from our red spectral data, which cover the wavelength range 6400–7200 A. In most cases, the detected emission line is Hα. The current survey list covers the region of the NOAO Deep Wide Field Survey (NDWFS). This survey covers two fields; the first is 3° × 3° and located at R.A. = 14h30m, δ = 34°30' (B1950.0), and the second is 23 × 40 and centered at R.A. = 2h7m30s, δ = -4°44'. A total area of 19.65 deg2 is covered by the KISS data. A total of 261 candidate emission-line objects have been selected for inclusion in the survey list (13.3 deg-2). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift, emission-line flux, and line equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS ELGs are examined using the available observational data. When combined with the wealth of multiwavelength data already available for the NDWFS fields, the current list of KISS ELGs should provide a valuable tool for studying star formation and nuclear activity in galaxies in the local universe.

Spectroscopy of KISS Emission-Line Galaxy Candidates. IV. KPNO and WIYN Observations

Spectroscopic observations for 614 emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS) have been obtained using the KPNO 2.1 m telescope and the WIYN 3.5 m telescope. KISS is a wide-field objective-prism survey for extragalactic emission-line objects that has cataloged over 2400 ELG candidates to date. Spectroscopic follow-up observations are being carried out at several telescopes to study the characteristics of the survey objects. We present the following data derived from the KPNO spectra: redshifts, reddening estimates, line equivalent widths, Hα line fluxes, and emission-line ratios. The galaxies have been classified based on their emission-line characteristics. The procedure for selecting the ELG candidates in KISS is found to be very reliable: the follow-up observations verify the presence of emission lines in 93% of the sample presented here. A comparison of objective-prism survey data—redshifts, Hα line fluxes, and equivalent widths—to the long-slit measurements shows good overall agreement.

Spectroscopy of KISS Emission-Line Galaxy Candidates. III. A Second Set of MDM Observations

Spectroscopic observations for 315 emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS) have been obtained using the MDM Observatory 2.4 m telescope on Kitt Peak. KISS is a wide-field objective-prism survey for extragalactic emission-line objects that has cataloged over 2200 ELG candidates to date. Spectroscopic follow-up observations are being carried out to study the characteristics of the survey objects. The observational data presented here include redshifts, reddening estimates, line equivalent widths, H? line fluxes, and emission-line ratios. The galaxies have been classified based on their emission-line characteristics. The procedure for selecting the ELG candidates in KISS is found to be very reliable: 93% of the candidates in this sample are verified to have emission lines. A comparison of objective-prism survey data?redshifts, H? line fluxes, and equivalent widths?to the long-slit measurements shows good overall agreement.

Luminous Compact Blue Galaxies in the Local Universe

We use the KPNO International Spectroscopic Survey (KISS) for emission-line galaxies to identify and describe a sample of local analogs to the luminous compact blue galaxies (LCBGs) that are observed to be abundant at intermediate and high redshift. The sample is selected using criteria believed effective at isolating true examples of LCBGs: SBe(B band) < 21.0 mag arcsec-2, MB < -18.5 (for H0 = 75 km s-1 Mpc-1), and B - V < 0.6. In addition, all LCBG candidates presented are selected to have star formation as their dominant form of activity. We examine the properties of our LCBGs and compare them with those of other KISS star-forming galaxies of the same absolute magnitude range. We find that the KISS LCBGs lie on the extreme end of a fairly continuous distribution of normal star-forming galaxies in the plane of surface brightness versus color. This result differs from the results of previous studies that show LCBGs at higher z to be more separate from the normal (usually nonactive) galaxies with which they are compared. On average, LCBGs have a higher tendency to emit detectable flux in the radio continuum; have higher Hα luminosities by a factor of 1.6, indicating strong star formation activity; and have slightly lower than expected metal abundances based on the luminosity-metallicity relation for KISS galaxies. We calculate the volume density of our low-z (z < 0.045) sample to be 5.4 × 10-4 h Mpc-3, approximately 4 times lower than the volume density of the LCBGs at 0.4 < z < 0.7 and ~10 times lower than the volume density of the population at 0.7 < z < 1.0.

Metal Abundances of KISS Galaxies. III. Nebular Abundances for Fourteen Galaxies and the Luminosity‐Metallicity Relationship for HiiGalaxies

We report results from the third in a series of nebular abundance studies of emission-line galaxies from the KPNO International Spectroscopic Survey (KISS). Galaxies with coarse metallicity estimates of 12 + log(O/H) less than 8.2 dex were selected for observation. Spectra of 14 galaxies, which cover the full optical region from [O II] λλ3727, 3729 to beyond [S II] λλ6717, 6731, are presented, and abundance ratios of N, O, Ne, S, and Ar are computed. The auroral [O III] λ4363 line is detected in all 14 galaxies. Oxygen abundances determined through the direct electron temperature (Te) method confirm that the sample is metal-poor with 7.61 ≤ 12 + log(O/H) ≤ 8.32. By using these abundances in conjunction with other Te-based measurements from the literature, we demonstrate that H II galaxies and more quiescent dwarf irregular galaxies follow similar metallicity-luminosity (L-Z) relationships. The primary difference is a zero-point shift between the correlations such that H II galaxies are brighter by an average of 0.8 B magnitudes at a given metallicity. This offset can be used as evidence to argue that low-luminosity H II galaxies typically undergo factor of 2 luminosity enhancements, and starbursts that elevate the luminosities of their host galaxies by 2-3 mag are not as common. We also demonstrate that the inclusion of interacting galaxies can increase the scatter in the L-Z relation and may force the observed correlation toward lower metallicities and/or larger luminosities. This must be taken into account when attempting to infer metal abundance evolution by comparing local L-Z relations with ones based on higher redshift samples, since the fraction of interacting galaxies should increase with look-back time.

Spectroscopy of KISS Emission-Line Galaxy Candidates. II. Hobby-Eberly Telescope Observations

The KPNO International Spectroscopic Survey (KISS) is an ongoing wide-field objective-prism survey for extragalactic emission-line objects. Over 2200 emission-line galaxy (ELG) candidates have been cataloged to date. To study the characteristics of the survey objects, spectroscopic follow-up observations are being carried out at several telescopes. Here we present the results of the spectroscopic observations for 258 KISS ELG candidates that have been obtained using the Marcario Low Resolution Spectrograph on the 9.2 m Hobby-Eberly Telescope (HET). We present the following data derived from the HET spectra: redshifts, reddening estimates, line equivalent widths, emission-line ratios, and galaxy activity types (e.g., AGN or star-forming). The long-slit redshifts are compared to those determined from the KISS objective-prism spectra and show good agreement. Earlier spectroscopic follow-up observations have typically verified the presence of emission lines for over 90% of the KISS ELG candidates. However, in the sample observed with the HET, only 78% of candidates are confirmed to be extragalactic emission-line sources. This is because the HET sample contains a large fraction of the faintest KISS objects, which typically have low spectral quality. A small number of objects at higher redshift (z ~ 0.3), detected by KISS from their [O III] emission rather than from Hα emission, are identified based on their spectra.

Radio Continuum Emission at 1.4 GHz from KISS Emission-Line Galaxies

We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST) and the NRAO VLA Sky Survey (NVSS) 1.4 GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (∼10%) in the first two Hα-selected survey lists were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z < 0.1). No dwarf galaxies were detected, despite the large numbers of low-luminosity galaxies present in KISS, suggesting that lower mass, lower luminosity objects do not possess strong galaxian-scale magnetic fields. Because of the selection technique used for KISS, our radio ELGs represent a quasi–volume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies). While there are many AGNs among the KISS radio galaxies, there are no objects with large radio powers in our local volume. We derive a radio luminosity function (RLF) for the KISS ELGs that agrees very well with previous RLFs that adequately sample the lower luminosity radio population.

The KPNO International Spectroscopic Survey. IV. H-selected Survey List 2

The KPNO International Spectroscopic Survey (KISS) is an objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the second list of emission-line galaxy candidates selected from our red spectral data, which cover the wavelength range 6400 to 7200 A. In most cases, the detected emission line is Hα. The current survey list covers a 16-wide strip located at δ = 43°30' (B1950) and spans the right ascension range 11h55m to 16h15m. The survey strip runs through the center of the Bootes void and has enough depth to adequately sample the far side of the void. An area of 65.8 deg2 is covered. A total of 1029 candidate emission-line objects have been selected for inclusion in the survey list (15.6 deg-2). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data. Although the current survey covers only a modest fraction of the total volume of the Bootes void, we catalog at least 12 objects that appear to be located within the void. Only one of these objects has been recognized previously as a void galaxy.

Metal Abundances of KISS Galaxies. II. Nebular Abundances of 12 Low-Luminosity Emission-Line Galaxies

We present follow-up spectra of 39 emission-line galaxies (ELGs) from the KPNO International Spectroscopic Survey (KISS). Many targets were selected as potentially low-metallicity systems based on their absolute B magnitudes and the metallicity-luminosity relation. The spectra, obtained with the Lick 3 m telescope, cover the full optical region from [O II] λλ3726, 3729 to beyond [S II] λλ6717, 6731 and include measurement of [O III] λ4363 in 12 objects. The spectra are presented and tables of the strong line ratios are given. For 12 high signal-to-noise ratio spectra, we determine abundance ratios of oxygen, nitrogen, neon, sulfur, and argon. We find these galaxies to be metal deficient with three systems approaching O/H of 1/25th solar. We compare the abundance results from the temperature-based Te method to the results from the strong-line p3 method of Pilyguin.

Spectroscopy of KISS Emission-Line Galaxy Candidates. I. MDM Observations

Spectroscopic observations for 351 emission-line galaxy candidates from the KPNO International Spectroscopic Survey (KISS) have been obtained using the MDM Observatory 2.4 m telescope on Kitt Peak. KISS is an ongoing wide-field objective-prism survey for extragalactic emission-line objects, which has cataloged over 2200 emission-line galaxy (ELG) candidates to date. Spectroscopic follow-up observations are being carried out to study the characteristics of the survey objects. The observational data presented here include redshifts, reddening estimates, line equivalent widths, Hα line fluxes, and emission-line ratios. The galaxies have been classified based on their emission-line characteristics. The procedure for selecting the ELG candidates in KISS is found to be very reliable: 95% of the candidates in this sample are verified to have emission lines. A comparison of objective-prism survey data—redshifts, Hα line fluxes, and equivalent widths—with the long-slit measurements shows good overall agreement.