260 research outputs found
Shocks or Photoionization: Direct Temperature Measurements of the Low-Ionization Gas in Quiescent Galaxies
The ionization mechanism of the low-ionization gas in quiescent red-sequence galaxies has been a long-standing puzzle. Direct temperature measurements would put strong constraints on this issue. We carefully selected a sample of quiescent red-sequence galaxies from Sloan Digital Sky Survey. We bin them into three bins with different [N II]/H α and [N II]/[O II] ratios, and we measure the temperature-sensitive [O III] λ4363, [N II] λ5755, [S II] λλ4068, 4076, and [O II] λλ7320, 7330 lines in the stacked spectra. The [S II] doublet ratios indicate the line-emitting gas is in the low-density regime (∼10–200 cm−3). We found the temperatures in the S+ zones to be around 8000 K, the temperatures in the O+ zone to be around 1.1–1.5 × 104 K, and the temperatures in the N+ zones to be around 1–1.4× 104 K. The [O III] λ4363 line is not robustly detected. We found that the extinction corrections derived from Balmer decrements would yield unphysical relationships between the temperatures of the S+ zones and O+ zones, indicating that the extinction is significantly overestimated by the measured Balmer decrements. We compared these line ratios with model predictions for three ionization mechanisms: photoionization by hot evolved stars, shocks, and turbulent mixing layers. For the photoionization and shock models, the hot temperatures inferred from [S ii] and [N II] coronal-to-strong line ratios require metallicities to be significantly subsolar. However, the [N II]/[O II] line ratios require them to be supersolar. None of the models could simultaneously explain all of the observed line ratios, neither could their combinations do
Nitrogen-to-Oxygen Abundance Ratio Variation In Quiescent Galaxies
For the first time, we establish a gas phase abundance pattern calibration
for quiescent galaxies using optical emission lines. Quiescent galaxies have
warm ionized gas showing line ratios similar to low-ionization nuclear emission
line regions (LINER). The ionization mechanism for the gas is still an
unsettled puzzle. Despite the uncertainty in the ionization mechanism, we argue
that we can still infer certain gas phase abundance pattern from first
principles. We show that the relative trend in N/O abundance can still be
reliably measured based on [NII]6548,6583/[OII]3726,3729 and a direct
measurement of the electron temperature. We construct a composite direct
temperature tracer that is independent of extinction correction, by combining
[OII] 3726,3729/[OII] 7320,7330 and [SII] 6716,6730/[SII] 4068,4076 and
canceling out the effect of extinction, as these involve the easiest-to-detect
auroral lines in quiescent galaxies. With theoretical modeling, we establish
the calibration for N/O based on [NII]/[OII] and a temperature tracer. We apply
this technique to quiescent galaxies in the nearby Universe and find they span
a range of 0.35 dex in N/O ratio from 17-percentile to 83-percentiles of the
whole distribution. These measurements can shed light on the chemical
enrichment history of the warm ionized gas in quiescent galaxies.Comment: 9 pages, 7 figures. Accepted for publication in MNRA
Shocks or Photoionization: Direct Temperature Measurements of the Low-Ionization Gas in Quiescent Galaxies
The ionization mechanism of the low-ionization gas in quiescent red sequence
galaxies has been a long-standing puzzle. Direct temperature measurements would
put strong constraints on this issue. We carefully selected a sample of
quiescent red sequence galaxies from SDSS. We bin them into three bins with
different [N II]/H{\alpha} and [N II]/[O II] ratios, and we measure the
temperature-sensitive [O III] {\lambda}4363, [N II] {\lambda}5755, [S II]
{\lambda}{\lambda}4068,4076, and [O II] {\lambda}{\lambda}7320,7330 lines in
the stacked spectra. The [S II] doublet ratios indicate the line-emitting gas
is in the low density regime (~10-100 cm).We found the temperatures in
the S+ zones to be around 8000K, the temperatures in the O+ zones to be around
K, and the temperatures in the N+ zones to be around
K. The [O III] {\lambda}4363 line is not robustly detected. We
found that the extinction corrections derived from Balmer decrements would
yield unphysical relationships between the temperatures of the S+ zones and O+
zones, indicating that the extinction is significantly overestimated by the
measured Balmer decrements. We compared these line ratios with model
predictions for three ionization mechanisms: photoionization by hot evolved
stars, shocks, and turbulent mixing layers. For both the photoionization and
shock models, the hot temperatures inferred from [S II] and [N II]
coronal-to-strong line ratios require metallicities to be significantly
subsolar. However, the [N II]/[O II] line ratios require them to be supersolar.
None of the models could simultaneously explain all of the observed line
ratios, neither could their combinations do.Comment: 20 pages, 17 figures. Accepted by MNRA
Nitrogen-to-Oxygen Abundance Ratio Variation in Quiescent Galaxies
For the first time, we establish a gas-phase abundance pattern calibration for quiescent galaxies using optical emission lines. Quiescent galaxies have warm ionized gas showing line ratios similar to low-ionization nuclear emission line regions. The ionization mechanism for the gas is still an unsettled puzzle. Despite the uncertainty in the ionization mechanism, we argue that we can still infer certain gas-phase abundance pattern from first principles. We show that the relative trend in N/O abundance can still be reliably measured based on [N II] λλ6548,6583/[O II] λλ3726,3729 and a direct measurement of the electron temperature. We construct a composite direct temperature tracer that is independent of extinction correction, by combining [O II] λλ3726,3729/[O II] λ7320,7330 and [S II] λλ6716,6731/[S II] λ4068,4076 and cancelling out the effect of extinction, as these involve the easiest-to-detect auroral lines in quiescent galaxies. With theoretical modelling, we establish the calibration for N/O based on [N II]/[O II] and a temperature tracer. We apply this technique to quiescent galaxies in the nearby Universe and find they span a range of 0.35 dex in N/O ratio from 17-percentile to 83-percentile of the whole distribution. These measurements can shed light on the chemical enrichment history of the warm ionized gas in quiescent galaxies
Stellar Metallicity Gradients in SDSS galaxies
We infer stellar metallicity and abundance ratio gradients for a sample of
red galaxies in the Sloan Digital Sky Survey (SDSS) Main galaxy sample. Because
this sample does not have multiple spectra at various radii in a single galaxy,
we measure these gradients statistically. We separate galaxies into stellar
mass bins, stack their spectra in redshift bins, and calculate the measured
absorption line indices in projected annuli by differencing spectra in
neighboring redshift bins. After determining the line indices, we use stellar
population modeling from the EZ\_Ages software to calculate ages,
metallicities, and abundance ratios within each annulus. Our data covers the
central regions of these galaxies, out to slightly higher than . We
find detectable gradients in metallicity and relatively shallow gradients in
abundance ratios, similar to results found for direct measurements of
individual galaxies. The gradients are only weakly dependent on stellar mass,
and this dependence is well-correlated with the change of with mass.
Based on this data, we report mean equivalent widths, metallicities, and
abundance ratios as a function of mass and velocity dispersion for SDSS
early-type galaxies, for fixed apertures of 2.5 kpc and of 0.5 .Comment: 19 pages; 8 tables, 12 figures. Submitted to ApJ for publicatio
Inside-out growth or inside-out quenching? clues from colour gradients of local galaxies
We constrain the spatial gradient of star formation history within galaxies
using the colour gradients in NUV-u and u-i for a local spatially-resolved
galaxy sample. By splitting each galaxy into an inner and an outer part, we
find that most galaxies show negative gradients in these two colours. We first
rule out dust extinction gradient and metallicity gradient as the dominant
source for the colour gradient. Then using stellar population models, we
explore variations in star formation history to explain the colour gradients.
As shown by our earlier work, a two-phase SFH consisting of an early secular
evolution (growth) phase and a subsequent rapid evolution (quenching) phase is
necessary to explain the observed colour distributions among galaxies. We
explore two different inside-out growth models and two different inside-out
quenching models by varying parameters of the SFH between inner and outer
regions of galaxies. Two of the models can explain the observed range of colour
gradients in NUV-u and u-i colours. We further distinguish them using an
additional constraint provided by the u-i colour gradient distribution, under
the assumption of constant galaxy formation rate and a common SFH followed by
most galaxies. We find the best model is an inside-out growth model in which
the inner region has a shorter e-folding time scale in the growth phase than
the outer region. More spatially resolved ultraviolet (UV) observations are
needed to improve the significance of the result.Comment: 11 pages, 7 figures, accepted for publication in MNRA
Metal-poor, Strongly Star-Forming Galaxies in the DEEP2 Survey: The Relationship between Stellar Mass, Temperature-based Metallicity, and Star Formation Rate
We report on the discovery of 28 metal-poor galaxies in DEEP2.
These galaxies were selected for their detection of the weak
[OIII]4363 emission line, which provides a "direct" measure of the
gas-phase metallicity. A primary goal for identifying these rare galaxies is to
examine whether the fundamental metallicity relation (FMR) between stellar
mass, gas metallicity, and star formation rate (SFR) holds for low stellar mass
and high SFR galaxies. The FMR suggests that higher SFR galaxies have lower
metallicity (at fixed stellar mass). To test this trend, we combine
spectroscopic measurements of metallicity and dust-corrected SFRs, with stellar
mass estimates from modeling the optical photometry. We find that these
galaxies are dex above the z~1 stellar mass-SFR relation, and
dex below the local mass-metallicity relation. Relative to the
FMR, the latter offset is reduced to 0.01 dex, but significant dispersion
remains (0.29 dex with 0.16 dex due to measurement uncertainties). This
dispersion suggests that gas accretion, star formation and chemical enrichment
have not reached equilibrium in these galaxies. This is evident by their short
stellar mass doubling timescale of Myr that suggests
stochastic star formation. Combining our sample with other z~1 metal-poor
galaxies, we find a weak positive SFR-metallicity dependence (at fixed stellar
mass) that is significant at 94.4% confidence. We interpret this positive
correlation as recent star formation that has enriched the gas, but has not had
time to drive the metal-enriched gas out with feedback mechanisms.Comment: Resubmitted to ApJ on March 6, 2015. Revised to discuss selection
biases and methodologies, and address the former by including more metal-rich
galaxies with robust non-detections of [OIII]4363. Primary results on FMR
analyses are unchanged. Additional figures are included to illustrate
selection biases; previous figures have been revised to improve presentatio
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