We present maps tracing the fraction of dust in the form of polycyclic aromatic hydrocarbons (PAHs) in IC 5332, NGC 628, NGC 1365, and NGC 7496 from JWST/MIRI observations. We trace the PAH fraction by combining the F770W (7.7
We present near and midinfrared (0.9–18
 Publication Date:
 NSFPAR ID:
 10390096
 Journal Name:
 The Astrophysical Journal Letters
 Volume:
 942
 Issue:
 1
 Page Range or eLocationID:
 Article No. L18
 ISSN:
 20418205
 Publisher:
 DOI PREFIX: 10.3847
 Sponsoring Org:
 National Science Foundation
More Like this

Abstract μ m) and F1130W (11.3μ m) filters to track ionized and neutral PAH emission, respectively, and comparing the PAH emission to F2100W, which traces small, hot dust grains. We find the averageR _{PAH}= (F770W + F1130W)/F2100W values of 3.3, 4.7, 5.1, and 3.6 in IC 5332, NGC 628, NGC 1365, and NGC 7496, respectively. We find that Hii regions traced by MUSE Hα show a systematically low PAH fraction. The PAH fraction remains relatively constant across other galactic environments, with slight variations. We use CO+Hi +Hα to trace the interstellar gas phase and find that the PAH fraction decreases above a value of in all four galaxies. Radial profiles also show a decreasing PAH fraction with increasing radius, correlated with lower metallicity, in line with previous results showing a strong metallicity dependence to the PAH fraction. Our results suggest that the process of PAH destruction in ionized gas operates similarlymore » ${\mathrm{I}}_{\mathrm{H}\alpha}/{\mathrm{\Sigma}}_{\mathrm{H}\mathrm{I}+{\mathrm{H}}_{2}}\sim {10}^{37.5}\phantom{\rule{0.25em}{0ex}}\mathrm{erg}\phantom{\rule{0.25em}{0ex}}{\mathrm{s}}^{1}\phantom{\rule{0.25em}{0ex}}{\mathrm{kpc}}^{2}\phantom{\rule{0.25em}{0ex}}{({M}_{\odot}\phantom{\rule{0.25em}{0ex}}{\mathrm{pc}}^{2})}^{1}$ 
Abstract We present a multiwavelength analysis of the galaxy cluster SPTCL J06074448 (SPT0607), which is one of the most distant clusters discovered by the South Pole Telescope at
z = 1.4010 ± 0.0028. The highredshift cluster shows clear signs of being relaxed with wellregulated feedback from the active galactic nucleus (AGN) in the brightest cluster galaxy (BCG). Using Chandra Xray data, we construct thermodynamic profiles and determine the properties of the intracluster medium. The coolcore nature of the cluster is supported by a centrally peaked density profile and low central entropy ( keV cm^{2}), which we estimate assuming an isothermal temperature profile due to the limited spectral information given the distance to the cluster. Using the density profile and gas cooling time inferred from the Xray data, we find a masscooling rate ${K}_{0}={18}_{9}^{+11}$ yr^{−1}. From optical spectroscopy and photometry around the [O ${\stackrel{\u0307}{M}}_{\mathrm{cool}}={100}_{60}^{+90}\phantom{\rule{0.25em}{0ex}}{M}_{\odot}$ii ] emission line, we estimate that the BCG star formation rate is yr^{−1}, roughly two orders of magnitude lower than the predicted masscooling rate. In addition, using ATCA radio data at 2.1 GHz, we measure a radio jet power ${\mathrm{SFR}}_{[\mathrm{O}\phantom{\rule{0.25em}{0ex}}\mathrm{II}]}={1.7}_{0.6}^{+1.0}\phantom{\rule{0.25em}{0ex}}{M}_{\odot}$ erg s^{−1}, which is consistent withmore » ${P}_{\mathrm{cav}}={3.2}_{1.3}^{+2.1}\times {10}^{44}$ 
Abstract We present the characteristics of 2 mm selected sources from the largest Atacama Large Millimeter/submillimeter Array (ALMA) blankfield contiguous survey conducted to date, the Mapping Obscuration to Reionization with ALMA (MORA) survey covering 184 arcmin^{2}at 2 mm. Twelve of 13 detections above 5
σ are attributed to emission from galaxies, 11 of which are dominated by cold dust emission. These sources have a median redshift of primarily based on optical/nearinfrared photometric redshifts with some spectroscopic redshifts, with 77% ± 11% of sources at $\u3008{z}_{2\phantom{\rule{0.25em}{0ex}}\mathrm{mm}}\u3009={3.6}_{0.3}^{+0.4}$z > 3 and 38% ± 12% of sources atz > 4. This implies that 2 mm selection is an efficient method for identifying the highestredshift dusty starforming galaxies (DSFGs). Lowerredshift DSFGs (z < 3) are far more numerous than those atz > 3 yet are likely to drop out at 2 mm. MORA shows that DSFGs with star formation rates in excess of 300M _{⊙}yr^{−1}and a relative rarity of ∼10^{−5}Mpc^{−3}contribute ∼30% to the integrated star formation rate density at 3 <z < 6. The volume density of 2 mm selected DSFGs is consistent with predictions from some cosmological simulations and is similar to the volume density of their hypothesized descendants: massive, quiescent galaxies atz > 2. Analysis of MORA sources’more » 
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 the discovery of the first millimeter afterglow of a shortduration
γ ray burst (SGRB) and the first confirmed afterglow of an SGRB localized by the GUANO system on Swift. Our Atacama Large Millimeter/Submillimeter Array (ALMA) detection of SGRB 211106A establishes an origin in a faint host galaxy detected in Hubble Space Telescope imaging at 0.7 ≲z ≲ 1.4. From the lack of a detectable optical afterglow, coupled with the bright millimeter counterpart, we infer a high extinction,A _{V}≳ 2.6 mag along the line of sight, making this one of the most highly dustextincted SGRBs known to date. The millimeterband light curve captures the passage of the synchrotron peak from the afterglow forward shock and reveals a jet break at days. For a presumed redshift of ${t}_{\mathrm{jet}}={29.2}_{4.0}^{+4.5}$z = 1, we infer an opening angle,θ _{jet}= (15.°5 ± 1.°4), and beamingcorrected kinetic energy of , making this one of the widest and most energetic SGRB jets known to date. Combining all published millimeterband upper limits in conjunction with the energetics for a large sample of SGRBs, we find that energetic outflows in highdensity environments are more likely to have detectable millimeter counterparts. Concerted afterglow searches with ALMA shouldmore » $\mathrm{log}({E}_{\mathrm{K}}/\mathrm{erg})=51.8\pm 0.3$