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<jats:title>Abstract</jats:title> <jats:p>We have analyzed Atacama Large Millimeter/submillimeter Array Cycle 4 Band 6 data toward two young stellar objects (YSOs), Oph-emb5 and Oph-emb9, in the Ophiuchus star-forming region. The YSO Oph-emb5 is located in a relatively quiescent region, whereas Oph-emb9 is irradiated by a nearby bright Herbig Be star. Molecular lines from <jats:italic>cyclic</jats:italic>-C<jats:sub>3</jats:sub>H<jats:sub>2</jats:sub> (<jats:italic>c</jats:italic>-C<jats:sub>3</jats:sub>H<jats:sub>2</jats:sub>), H<jats:sub>2</jats:sub>CO, CH<jats:sub>3</jats:sub>OH, <jats:sup>13</jats:sup>CO, C<jats:sup>18</jats:sup>O, and DCO<jats:sup>+</jats:sup> have been detected from both sources, while DCN is detected only in Oph-emb9. Around Oph-emb5, <jats:italic>c</jats:italic>-C<jats:sub>3</jats:sub>H<jats:sub>2</jats:sub> is enhanced at the west side, relative to the IR source, whereas H<jats:sub>2</jats:sub>CO and CH<jats:sub>3</jats:sub>OH are abundant at the east side. In the field of Oph-emb9, moment 0 maps of the <jats:italic>c</jats:italic>-C<jats:sub>3</jats:sub>H<jats:sub>2</jats:sub> lines show a peak at the eastern edge of the field of view, which is irradiated by the Herbig Be star. Moment 0 maps of CH<jats:sub>3</jats:sub>OH and H<jats:sub>2</jats:sub>CO show peaks farther from the bright star. We derive the <jats:italic>N</jats:italic>(<jats:italic>c</jats:italic>-C<jats:sub>3</jats:sub>H<jats:sub>2</jats:sub>)/<jats:italic>N</jats:italic>(CH<jats:sub>3</jats:sub>OH) column density ratios at the peak positions of <jats:italic>c</jats:italic>-C<jats:sub>3</jats:sub>H<jats:sub>2</jats:sub> and CH<jats:sub>3</jats:sub>OH near each YSO, which are identified based on their moment 0 maps. The <jats:italic>N</jats:italic>(<jats:italic>c</jats:italic>-C<jats:sub>3</jats:sub>H<jats:sub>2</jats:sub>)/<jats:italic>N</jats:italic>(CH<jats:sub>3</jats:sub>OH) ratio at the <jats:italic>c</jats:italic>-C<jats:sub>3</jats:sub>H<jats:sub>2</jats:sub> peak is significantly higher than at the CH<jats:sub>3</jats:sub>OH peak by a factor of ∼19 in Oph-emb9, while the difference in this column density ratio between these two positions is a factor of ∼2.6 in Oph-emb5. These differences are attributed to the efficiency of the photon-dominated region chemistry in Oph-emb9. The higher DCO<jats:sup>+</jats:sup> column density and the detection of DCN in Oph-emb9 are also discussed in the context of UV irradiation flux.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Low-density points (LDPs), obtained by removing high-density regions of observed galaxies, can trace the large-scale structures (LSSs) of the universe. In particular, it offers an intriguing opportunity to detect weak gravitational lensing from low-density regions. In this work, we investigate the tomographic cross-correlation between Planck cosmic microwave background (CMB) lensing maps and LDP-traced LSSs, where LDPs are constructed from the DR8 data release of the DESI legacy imaging survey, with about 10<jats:sup>6</jats:sup>–10<jats:sup>7</jats:sup> galaxies. We find that, due to the large sky coverage (20,000 deg<jats:sup>2</jats:sup>) and large redshift depth (<jats:italic>z</jats:italic> ≤ 1.2), a significant detection (10<jats:italic>σ</jats:italic>–30<jats:italic>σ</jats:italic>) of the CMB lensing–LDP cross-correlation in all six redshift bins can be achieved, with a total significance of ∼53<jats:italic>σ</jats:italic> over <jats:italic>ℓ</jats:italic> ≤ 1024. Moreover, the measurements are in good agreement with a theoretical template constructed from our numerical simulation in the WMAP 9 yr ΛCDM cosmology. A scaling factor for the lensing amplitude <jats:italic>A</jats:italic> <jats:sub>lens</jats:sub> is constrained to <jats:italic>A</jats:italic> <jats:sub>lens</jats:sub> = 1 ± 0.12 for <jats:italic>z</jats:italic> &lt; 0.2, <jats:italic>A</jats:italic> <jats:sub>lens</jats:sub> = 1.07 ± 0.07 for 0.2 &lt; <jats:italic>z</jats:italic> &lt; 0.4, and <jats:italic>A</jats:italic> <jats:sub>lens</jats:sub> = 1.07 ± 0.05 for 0.4 &lt; <jats:italic>z</jats:italic> &lt; 0.6, with the <jats:italic>r</jats:italic>-band absolute magnitude cut of −21.5 for LDP selection. A variety of tests have been performed to check the detection reliability against variations in LDP samples and galaxy magnitude cuts, masks, CMB lensing maps, multipole <jats:italic>ℓ</jats:italic> cuts, sky regions, and photo-<jats:italic>z</jats:italic> bias. We also perform a cross-correlation measurement between CMB lensing and galaxy number density, which is consistent with the CMB lensing–LDP cross-correlation. This work therefore further convincingly demonstrates that LDP is a competitive tracer of LSS.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) will produce several billion photometric redshifts (photo-<jats:italic>z</jats:italic>'s), enabling cosmological analyses to select a subset of galaxies with the most accurate photo-<jats:italic>z</jats:italic>. We perform initial redshift fits on Subaru Strategic Program galaxies with deep <jats:italic>grizy</jats:italic> photometry using Trees for Photo-Z (TPZ) before applying a custom neural network classifier (NNC) tuned to select galaxies with (<jats:italic>z</jats:italic> <jats:sub>phot</jats:sub> − <jats:italic>z</jats:italic> <jats:sub>spec</jats:sub>)/(1 + <jats:italic>z</jats:italic> <jats:sub>spec</jats:sub>) &lt; 0.10. We consider four cases of training and test sets ranging from an idealized case to using data augmentation to increase the representation of dim galaxies in the training set. Selections made using the NNC yield significant further improvements in outlier fraction and photo-<jats:italic>z</jats:italic> scatter (<jats:italic>σ</jats:italic> <jats:sub> <jats:italic>z</jats:italic> </jats:sub>) over those made with typical photo-<jats:italic>z</jats:italic> uncertainties. As an example, when selecting the best third of the galaxy sample, the NNC achieves a 35% improvement in outlier rate and a 23% improvement in <jats:italic>σ</jats:italic> <jats:sub> <jats:italic>z</jats:italic> </jats:sub> compared to using uncertainties from TPZ. For cosmology and galaxy evolution studies, this method can be tuned to retain a particular sample size or to achieve a desired photo-<jats:italic>z</jats:italic> accuracy; our results show that it is possible to retain more than a third of an LSST-like galaxy sample while reducing <jats:italic>σ</jats:italic> <jats:sub> <jats:italic>z</jats:italic> </jats:sub> by a factor of 2 compared to the full sample, with one-fifth as many photo-<jats:italic>z</jats:italic> outliers. For surveys like LSST that are not limited by shot noise, this method enables a larger number of tomographic redshift bins and hence a significant increase in the total signal to noise of galaxy angular power spectra.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We apply a new galaxy group-finder to the Main Galaxy Sample of the SDSS. This algorithm introduces new freedom to assign halos to galaxies that is self-calibrated by comparing the catalog to complementary data. These include galaxy clustering data and measurements of the total satellite luminosity from deep-imaging data. We present constraints on the galaxy-halo connection for star-forming and quiescent populations. The results of the self-calibrated group catalog differ in several key ways from previous group catalogs and halo-occupation analyses. The transition halo mass scale, where half of the halos contain quiescent central galaxies, is at <jats:italic>M</jats:italic> <jats:sub> <jats:italic>h</jats:italic> </jats:sub> ∼ 10<jats:sup>12.4</jats:sup> <jats:italic>h</jats:italic> <jats:sup>−1</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>, significantly higher than other constraints. Additionally, the width of the transition from predominantly star-forming halos to quiescent halos occurs over a narrower range in halo mass. Quiescent central galaxies in low-mass halos are significantly more massive than star-forming centrals at the same halo mass, but this difference reverses above the transition halo mass. We find that the scatter in <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{log}{M}_{* }$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>log</mml:mi> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac2aaaieqn1.gif" xlink:type="simple" /> </jats:inline-formula> at fixed <jats:italic>M</jats:italic> <jats:sub> <jats:italic>h</jats:italic> </jats:sub> is ∼0.2 dex for massive halos, in agreement with previous estimates, but rises sharply at lower halo masses. The halo masses assigned by the group catalog are in good agreement with weak-lensing estimates for star-forming and quiescent central galaxies. We discuss possible improvements to the algorithm made clear by this first application to data. The group catalog is made publicly available.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present the full panchromatic afterglow light-curve data of GW170817, including new radio data as well as archival optical and X-ray data, between 0.5 and 940 days post-merger. By compiling all archival data and reprocessing a subset of it, we have evaluated the impact of differences in data processing or flux determination methods used by different groups and attempted to mitigate these differences to provide a more uniform data set. Simple power-law fits to the uniform afterglow light curve indicate a <jats:italic>t</jats:italic> <jats:sup>0.86±0.04</jats:sup> rise, a <jats:italic>t</jats:italic> <jats:sup>−1.92±0.12</jats:sup> decline, and a peak occurring at 155 ± 4 days. The afterglow is optically thin throughout its evolution, consistent with a single spectral index (−0.584 ± 0.002) across all epochs. This gives a precise and updated estimate of the electron power-law index, <jats:italic>p</jats:italic> = 2.168 ± 0.004. By studying the diffuse X-ray emission from the host galaxy, we place a conservative upper limit on the hot ionized interstellar medium density, &lt;0.01 cm<jats:sup>−3</jats:sup>, consistent with previous afterglow studies. Using the late-time afterglow data we rule out any long-lived neutron star remnant having a magnetic field strength between 10<jats:sup>10.4</jats:sup> and 10<jats:sup>16</jats:sup> G. Our fits to the afterglow data using an analytical model that includes Very Long Baseline Interferometry proper motion from Mooley et al., and a structured jet model that ignores the proper motion, indicates that the proper-motion measurement needs to be considered when seeking an accurate estimate of the viewing angle.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We report the detection of more than 120 emission lines corresponding to eight complex organic molecules (COMs; CH<jats:sub>3</jats:sub>OH, CH<jats:sub>3</jats:sub>CH<jats:sub>2</jats:sub>OH, CH<jats:sub>3</jats:sub>OCH<jats:sub>3</jats:sub>, CH<jats:sub>3</jats:sub>OCHO, CH<jats:sub>3</jats:sub>COCH<jats:sub>3</jats:sub>, NH<jats:sub>2</jats:sub>CHO, CH<jats:sub>2</jats:sub>DCN, and CH<jats:sub>3</jats:sub>CH<jats:sub>2</jats:sub>CN) and three isotopologues (CH<jats:sub>2</jats:sub>DOH, <jats:sup>13</jats:sup>CH<jats:sub>3</jats:sub>CN, and CH<jats:sub>3</jats:sub>C<jats:sup>15</jats:sup>N) toward the western component of the Ser-emb 11 binary young stellar object using observations with the Atacama Large Millimeter/submillimeter Array at ∼1 mm. The complex organic emission was unresolved with a ∼0.″5 beam (∼220 au) in a compact region around the central protostar, and a population diagram analysis revealed excitation temperatures above 100 K for all COMs, indicating the presence of a hot corino. The estimated column densities were in the range of 10<jats:sup>17</jats:sup>−10<jats:sup>18</jats:sup> cm<jats:sup>−2</jats:sup> for the O-bearing COMs, and three orders of magnitude lower for the N-bearing species. We also report the detection of H<jats:sub>2</jats:sub>CO and CH<jats:sub>3</jats:sub>OH emission in a nearby millimeter source that had not been previously cataloged. Ser-emb 11 is classified in the literature as a Class I source near the Class 0/I cutoff. The estimated COM relative abundances in Ser-emb 11 W and the other three Class I hot corino sources reported in the literature are consistent with those of Class 0 hot corinos, suggesting a continuity in the chemical composition of hot corinos during protostellar evolution.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The massive black hole (BH) population in dwarf galaxies (<jats:italic>M</jats:italic> <jats:sub>BH</jats:sub> ≲ 10<jats:sup>5</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>) can provide strong constraints on the origin of BH seeds. However, traditional optical searches for active galactic nuclei (AGNs) only reliably detect high-accretion, relatively high-mass BHs in dwarf galaxies with low amounts of star formation, leaving a large portion of the overall BH population in dwarf galaxies relatively unexplored. Here, we present a sample of 81 dwarf galaxies (<jats:italic>M</jats:italic> <jats:sub>⋆</jats:sub> ≤ 3 × 10<jats:sup>9</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>) with detectable [Fe <jats:sc>x</jats:sc>]<jats:italic>λ</jats:italic>6374 coronal line emission indicative of accretion onto massive BHs, only two of which were previously identified as optical AGNs. We analyze optical spectroscopy from the Sloan Digital Sky Survey and find [Fe <jats:sc>x</jats:sc>]<jats:italic>λ</jats:italic>6374 luminosities in the range <jats:italic>L</jats:italic> <jats:sub>[Fe x]</jats:sub> ≈ 10<jats:sup>36</jats:sup>–10<jats:sup>39</jats:sup> erg s<jats:sup>−1</jats:sup>, with a median value of 1.6 × 10<jats:sup>38</jats:sup> erg s<jats:sup>−1</jats:sup>. The [Fe <jats:sc>x]</jats:sc> <jats:italic>λ</jats:italic>6374 luminosities are generally much too high to be produced by stellar sources, including luminous Type IIn supernovae (SNe). Moreover, based on known SNe rates, we expect at most eight Type IIn SNe in our sample. That said, the [Fe <jats:sc>x</jats:sc>]<jats:italic>λ</jats:italic>6374 luminosities are consistent with accretion onto massive BHs from AGNs or tidal disruption events (TDEs). We find additional indicators of BH accretion in some cases using other emission line diagnostics, optical variability, and X-ray and radio emission (or some combination of these). However, many of the galaxies in our sample only have evidence for a massive BH based on their [Fe <jats:sc>x</jats:sc>]<jats:italic>λ</jats:italic>6374 luminosities. This work highlights the power of coronal line emission to find BHs in dwarf galaxies missed by other selection techniques and to probe the BH population in bluer, lower-mass dwarf galaxies.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We identify a sample of spectroscopically measured emission line galaxy (ELG) Pairs up to <jats:italic>z</jats:italic> = 1.6 from the Wide Field Camera 3 (WFC3) Infrared Spectroscopic Parallels (WISP) survey. WISP obtained slitless, near-infrared grism spectroscopy along with direct imaging in the <jats:italic>J</jats:italic> and <jats:italic>H</jats:italic> bands by observing in the pure-parallel mode with the WFC3 on board the Hubble Space Telescope. From our search of 419 WISP fields covering an area of ∼0.5 deg<jats:sup>2</jats:sup>, we find 413 ELG pair systems, mostly H<jats:sub> <jats:italic>α</jats:italic> </jats:sub> emitters. We then derive reliable star formation rates (SFRs) based on the attenuation-corrected H<jats:sub> <jats:italic>α</jats:italic> </jats:sub> fluxes. Compared to isolated galaxies, we find an average SFR enhancement of 40%–65%, which is stronger for major Pairs and Pairs with smaller velocity separations (Δ<jats:sub> <jats:italic>v</jats:italic> </jats:sub> &lt; 300 km s<jats:sup>−1</jats:sup>). Based on the stacked spectra from various subsamples, we study the trends of emission line ratios in pairs, and find a general consistency with enhanced lower ionization lines. We study the pair fraction among ELGs, and find a marginally significant increase with redshift <jats:italic>f</jats:italic> ∝ (1 + <jats:italic>z</jats:italic>)<jats:sup> <jats:italic>α</jats:italic> </jats:sup>, where the power-law index <jats:italic>α</jats:italic> = 0.58 ± 0.17 from <jats:italic>z</jats:italic> ∼ 0.2 to ∼1.6. The fraction of active galactic nuclei is found to be the same in the ELG Pairs as compared to the isolated ELGs.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Ionization sources other than H <jats:sc>ii</jats:sc> regions give rise to the right-hand branch in the standard ([N <jats:sc>ii</jats:sc>]) BPT diagram, populated by Seyfert 2s and LINERs. However, because the majority of Seyfert/LINER hosts are star-forming (SF), H <jats:sc>ii</jats:sc> regions contaminate the observed lines to some extent, making it unclear if the position along the branch is merely due to various degrees of mixing between pure Seyferts/LINERs and SF, or whether it reflects the intrinsic diversity of Seyfert/LINER ionizing sources. In this study, we empirically remove SF contributions in ∼100,000 Seyferts/LINERs from SDSS using the doppelganger method. We find that mixing is not the principal cause of the extended morphology of the observed branch. Rather, Seyferts/LINERs intrinsically have a wide range of line ratios. Variations in ionization parameter and metallicity can account for much of the diversity of Seyfert/LINER line ratios, but the hardness of the ionization field also varies significantly. Furthermore, our <jats:italic>k</jats:italic>-means classification on seven decontaminated emission lines reveals that LINERs are made up of two populations, which we call soft and hard LINERs. The Seyfert 2s differ from both types of LINERs primarily by higher ionization parameter, whereas the two LINER types mainly differ from each other (and from star-forming regions) in the hardness of the radiation field. We confirm that the [N <jats:sc>ii</jats:sc>] BPT diagram more efficiently identifies LINERs than [S <jats:sc>ii</jats:sc>] and [O <jats:sc>i</jats:sc>] diagnostics, because in the latter many LINERs, especially soft ones, occupy the same location as pure starformers, even after the SF has been removed from LINER emission.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The recently developed J-region asymptotic giant branch (JAGB) method has extraordinary potential as an extragalactic standard candle, capable of calibrating the absolute magnitudes of locally accessible Type Ia supernovae, thereby leading to an independent determination of the Hubble constant. Using Gaia Early Data Release 3 (EDR3) parallaxes, we calibrate the zero-point of the JAGB method, based on the mean luminosity of a color-selected subset of carbon-rich AGB stars. We identify Galactic carbon stars from the literature and use their near-infrared photometry and Gaia EDR3 parallaxes to measure their absolute <jats:italic>J</jats:italic>-band magnitudes. Based on these Milky Way parallaxes we determine the zero-point of the JAGB method to be <jats:italic>M</jats:italic> <jats:sub> <jats:italic>J</jats:italic> </jats:sub> = −6.14 ± 0.05 (stat) ± 0.11 (sys) mag. This Galactic calibration serves as a consistency check on the JAGB zero-point, agreeing well with previously published, independent JAGB calibrations based on geometric, detached eclipsing binary distances to the LMC and SMC. However, the JAGB stars used in this study suffer from the high parallax uncertainties that afflict the bright and red stars in EDR3, so we are not able to attain the higher precision of previous calibrations, and ultimately will rely on future improved DR4 and DR5 releases.</jats:p>