We use ALMA observations of CO(2–1) in 13 massive (
Both thin (55
 Publication Date:
 NSFPAR ID:
 10415619
 Journal Name:
 Journal of The Electrochemical Society
 Volume:
 170
 Issue:
 5
 Page Range or eLocationID:
 Article No. 050534
 ISSN:
 00134651
 Publisher:
 The Electrochemical Society
 Sponsoring Org:
 National Science Foundation
More Like this

Abstract M _{*}≳ 10^{11}M _{⊙}) poststarburst galaxies atz ∼ 0.6 to constrain the molecular gas content in galaxies shortly after they quench their major starforming episode. The poststarburst galaxies in this study are selected from the Sloan Digital Sky Survey spectroscopic samples (Data Release 14) based on their spectral shapes, as part of the Studying QUenching at Intermediatez Galaxies: Gas, angu momentum, and Evolution ( $$\overrightarrow{L}\mathrm{ar}$$ ) program. Early results showed that two poststarburst galaxies host large H_{2}reservoirs despite their low inferred star formation rates (SFRs). Here we expand this analysis to a larger statistical sample of 13 galaxies. Six of the primary targets (45%) are detected, with $\mathit{SQuIGG}\stackrel{\u20d7}{L}E$ ${M}_{{\mathrm{H}}_{2}}\gtrsim {10}^{9}$M _{⊙}. Given their high stellar masses, this mass limit corresponds to an average gas fraction of or ∼14% using lower stellar masses estimates derived from analytic, exponentially declining star formation histories. The gas fraction correlates with the $\u3008{f}_{{\mathrm{H}}_{2}}\equiv {M}_{{\mathrm{H}}_{2}}/{M}_{*}\u3009\sim 7\%$D _{n}4000 spectral index, suggesting that the cold gas reservoirs decrease with time since burst, as found in local K+A galaxies. Star formation histories derived from flexible stellar population synthesis modeling support thismore » 
Abstract We investigate the stellar mass–black hole mass (
) relation with type 1 active galactic nuclei (AGNs) down to ${\mathit{\ue239}}_{*}\u2013{\mathit{\ue239}}_{\mathrm{BH}}$ , corresponding to a ≃ −21 absolute magnitude in restframe ultraviolet, at ${\mathit{\ue239}}_{\mathrm{BH}}={10}^{7\phantom{\rule{0.11em}{0ex}}}{M}_{\odot}$z = 2–2.5. Exploiting the deep and largearea spectroscopic survey of the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX), we identify 66 type 1 AGNs with ranging from 10^{7}–10^{10} ${\mathit{\ue239}}_{\mathrm{BH}}$M _{⊙}that are measured with singleepoch virial method using Civ emission lines detected in the HETDEX spectra. of the host galaxies are estimated from optical to nearinfrared photometric data taken with Spitzer, the Widefield Infrared Survey Explorer, and groundbased 4–8 m class telescopes by ${\mathit{\ue239}}_{*}$CIGALE spectral energy distribution (SED) fitting. We further assess the validity of SED fitting in two cases by hostnuclear decomposition performed through surface brightness profile fitting on spatially resolved host galaxies with the James Webb Space Telescope/NIRCam CEERS data. We obtain the relation covering the unexplored lowmass ranges of ${\mathit{\ue239}}_{*}\u2013{\mathit{\ue239}}_{\mathrm{BH}}$ , and conduct forward modeling to fully account for the selection biases and observational uncertainties. The intrinsic ${\mathit{\ue239}}_{\mathrm{BH}}\phantom{\rule{0.25em}{0ex}}\sim \phantom{\rule{0.25em}{0ex}}{10}^{7}\u2013{10}^{8}\phantom{\rule{0.25em}{0ex}}{M}_{\odot}$ relation at ${\mathit{\ue239}}_{*}\u2013{\mathit{\ue239}}_{\mathrm{BH}}$z ∼ 2 has a moderate positive offset ofmore » 
Abstract The genericity of Arnold diffusion in the analytic category is an open problem. In this paper, we study this problem in the following
a priori unstable Hamiltonian system with a timeperiodic perturbation where ${\mathcal{H}}_{\epsilon}(p,q,I,\phi ,t)=h(I)+\sum _{i=1}^{n}\pm \left(\frac{1}{2}{p}_{i}^{2}+{V}_{i}({q}_{i})\right)+\epsilon {H}_{1}(p,q,I,\phi ,t),$ , $(p,q)\in {\mathbb{R}}^{n}\times {\mathbb{T}}^{n}$ with $(I,\phi )\in {\mathbb{R}}^{d}\times {\mathbb{T}}^{d}$n ,d ⩾ 1,V _{i}are Morse potentials, andɛ is a small nonzero parameter. The unperturbed Hamiltonian is not necessarily convex, and the induced inner dynamics does not need to satisfy a twist condition. Using geometric methods we prove that Arnold diffusion occurs for generic analytic perturbationsH _{1}. Indeed, the set of admissibleH _{1}isC ^{ω}dense andC ^{3}open (a fortiori ,C ^{ω}open). Our perturbative technique for the genericity is valid in theC ^{k}topology for allk ∈ [3, ∞) ∪ {∞,ω }. 
Abstract We present^{13}CO(
J = 1 → 0) observations for the EDGECALIFA survey, which is a mapping survey of 126 nearby galaxies at a typical spatial resolution of 1.5 kpc. Using detected^{12}CO emission as a prior, we detect^{13}CO in 41 galaxies via integrated line flux over the entire galaxy and in 30 galaxies via integrated line intensity in resolved synthesized beams. Incorporating our CO observations and optical IFU spectroscopy, we perform a systematic comparison between the line ratio and the properties of the stars and ionized gas. Higher ${\mathit{\ue23e}}_{12/13}\equiv I{[}^{12}\mathrm{CO}(J=1\to 0)]/I{[}^{13}\mathrm{CO}(J=1\to 0)]$ values are found in interacting galaxies compared to those in noninteracting galaxies. The global ${\mathit{\ue23e}}_{12/13}$ slightly increases with infrared color ${\mathit{\ue23e}}_{12/13}$F _{60}/F _{100}but appears insensitive to other hostgalaxy properties such as morphology, stellar mass, or galaxy size. We also present azimuthally averaged profiles for our sample up to a galactocentric radius of 0.4 ${\mathit{\ue23e}}_{12/13}$r _{25}(∼6 kpc), taking into account the^{13}CO nondetections by spectral stacking. The radial profiles of are quite flat across our sample. Within galactocentric distances of 0.2 ${\mathit{\ue23e}}_{12/13}$r _{25}, the azimuthally averaged increases with the star formationmore » ${\mathit{\ue23e}}_{12/13}$ 
Abstract We present a Keck/MOSFIRE restoptical composite spectrum of 16 typical gravitationally lensed starforming dwarf galaxies at 1.7 ≲
z ≲ 2.6 (z _{mean}= 2.30), all chosen independent of emissionline strength. These galaxies have a median stellar mass of and a median star formation rate of $\mathrm{log}{({M}_{*}/{M}_{\odot})}_{\mathrm{med}}={8.29}_{0.43}^{+0.51}$ . We measure the faint electrontemperaturesensitive [O ${\mathrm{S}\mathrm{F}\mathrm{R}}_{\mathrm{H}\alpha}^{\mathrm{m}\mathrm{e}\mathrm{d}}={2.25}_{1.26}^{+2.15}\phantom{\rule{0.25em}{0ex}}{M}_{\odot}\phantom{\rule{0.25em}{0ex}}{\mathrm{y}\mathrm{r}}^{1}$iii ]λ 4363 emission line at 2.5σ (4.1σ ) significance when considering a bootstrapped (statisticalonly) uncertainty spectrum. This yields a directmethod oxygen abundance of ( $12+\mathrm{log}{(\mathrm{O}/\mathrm{H})}_{\mathrm{direct}}={7.88}_{0.22}^{+0.25}$ ). We investigate the applicability at high ${0.15}_{0.06}^{+0.12}\phantom{\rule{0.33em}{0ex}}{Z}_{\odot}$z of locally calibrated oxygenbased strongline metallicity relations, finding that the local reference calibrations of Bian et al. best reproduce (≲0.12 dex) our composite metallicity at fixed strongline ratio. At fixedM _{*}, our composite is well represented by thez ∼ 2.3 directmethod stellar mass—gasphase metallicity relation (MZR) of Sanders et al. When comparing to predicted MZRs from the IllustrisTNG and FIRE simulations, having recalculated our stellar masses with more realistic nonparametric star formation histories , we find excellent agreement with the FIRE MZR. Our composite is consistent with no metallicity evolution, atmore » $(\mathrm{log}{({M}_{*}/{M}_{\odot})}_{\mathrm{med}}={8.92}_{0.22}^{+0.31})$