{"total":13,"items":[{"citing_arxiv_id":"2606.30488","ref_index":59,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"High-Resolution Spectroscopy of Raman-scattered He II Lines in the Symbiotic Nova RR Telescopii","primary_cat":"astro-ph.SR","submitted_at":"2026-06-29T15:53:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Observations of Raman-scattered He II lines in RR Telescopii reveal distinct velocities tracing different H I depths and temporal declines in conversion efficiency, implying the neutral region needs complex radiative transfer models beyond a single column density.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28257","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"When Jets Don't Quench: Near-Infrared H$_{2}$ in Star Forming Low-Excitation Radio Galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-26T16:41:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New Gemini/GNIRS observations of star-forming radio galaxies show warm H2 emission driven primarily by mergers rather than jets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27245","ref_index":112,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"MUSE Imaging Spectroscopy of the Fullerene Planetary Nebula Tc 1","primary_cat":"astro-ph.SR","submitted_at":"2026-06-25T16:33:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"MUSE observations of Tc 1 map structured extinction, Te, and Ne, revealing a low-extinction annulus outside the main fullerene zone that is interpreted as evidence for locally altered dust properties in the core-halo transition.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25896","ref_index":39,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Two years of shock interaction tracing three phases of evolution: the explosion of a Type IIn supernova, SN 2019vxm","primary_cat":"astro-ph.HE","submitted_at":"2026-06-24T14:45:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Multi-wavelength observations of SN 2019vxm trace three phases of shock interaction in a Type IIn supernova, estimating CSM mass of 3-8 solar masses and ejecta mass of ~3.88 solar masses with late-time dust signatures.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13202","ref_index":66,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The first hours and days of the 2021 explosion of the recurrent symbiotic nova RS Ophiuchii","primary_cat":"astro-ph.SR","submitted_at":"2026-06-11T11:12:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"SED modeling of early 2021 RS Oph data indicates bipolar ejecta with equatorial disk and confirms significant WD radiation originates from reprocessed shock emission explained by WD rotation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12249","ref_index":182,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Spatially Resolved Nebular-Stellar Reddening with JWST/NIRISS","primary_cat":"astro-ph.GA","submitted_at":"2026-06-10T15:52:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST observations of high-redshift galaxies show no evolution in dust geometry to z~2.4 and yield an empirical calibration linking resolved differential reddening to SFR surface density.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19413","ref_index":89,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Gaia21bja: pre-main sequence star with quasi-periodic bursts","primary_cat":"astro-ph.SR","submitted_at":"2026-05-19T06:06:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Gaia21bja is identified as a pre-main sequence star with quasi-periodic bursts, showing spectral features and a 5.5-6 times higher accretion rate during outbursts that place it in the periodic category of outbursting YSOs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.03124","ref_index":203,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Nowhere Left to Hide: Uncovering All of the Massive Young Embedded Star Clusters in the Antennae with JWST","primary_cat":"astro-ph.GA","submitted_at":"2026-05-04T20:04:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST observations identify all massive young embedded star clusters in the Antennae, revealing they are extremely young, heavily obscured, and account for ~60% of the ionizing luminosity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.01105","ref_index":166,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Resolving the Unresolved Galactic Winds in Multi-phase Models. I. Methodology and Application","primary_cat":"astro-ph.GA","submitted_at":"2026-05-01T21:20:47+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A new fitting methodology applied to UV absorption data recovers radial trends in galactic wind velocities and mass-loading factors by constraining initial hot and cool phase parameters in a multiphase model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16822","ref_index":19,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dense Ionized Outflow with Five Narrow Components in a Dust-obscured Galaxy","primary_cat":"astro-ph.GA","submitted_at":"2026-04-18T04:27:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The dust-obscured galaxy J1010+3725 hosts a complex ionized outflow consisting of five narrow components with velocities from -1475 to +507 km/s and high hydrogen densities above 10^5 cm^{-3}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.01326","ref_index":75,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Calibrating Photometric Mid-Infrared Star Formation Rates for JWST","primary_cat":"astro-ph.GA","submitted_at":"2026-04-01T19:08:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Rest-frame 6-8um MIRI luminosity provides broken power-law SFR calibrations with 0.2-0.3 dex scatter and UV+IR composites at 0.15 dex, supporting robust use above log M* ~9 up to z~3.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"which may indicate they act as catalysts for the formation of H2 molecules (e.g., Bauschlicher 1998; Foley et al. 2018; Barrera et al. 2023). PAHs are also tightly correlated with star formation on scales from HII regions to entire galaxies (Calzetti et al. 2007). As bright features, PAHs in aggregate typically con- tribute ∼ 10% of the total infrared emission ( LIR ≡ L[8 − 1000µm Wu et al. 2010; Shipley et al. 2016) and up to∼ 20% in extreme cases (Smith et al. 2007). As such, PAHs− along with the rest-frame mid-IR continuum − have a prolific his- tory as a robust measure of the obscured SFR component (Le Floc'h et al. 2005; Reddy et al. 2006; Elbaz et al. 2011; Magnelli et al. 2011; Wuyts et al. 2011; Whitaker et al. 2012, 2017; Rujopakarn et al. 2013; Shipley et al. 2016; Cluver et al. 2017; Mahajan et al. 2019; Kov 'acs et al. 2019). This has been especially vital at higher redshifts, as previous in- struments such as Spitzer/MIPS at 24µm (Rieke et al. 2004) directly probed the rest-frame 8µm spectral region during cosmic noon. The catch, however, is that these studies have largely fo- cused on massive SFGs with roughly solar metallicities, where PAHs are ubiquitous (Elbaz et al. 2005; Yan et al. 2005; Sajina et al. 2007) and relatively well behaved. In these galaxies, stellar energy is largely absorbed and re-radiated by dust, such that the total infrared luminosity is closely repre- sentative of the bolometric luminosity of young stars, making it an excellent proxy not only for the obscured SFR but also the total SFR (Kennicutt & Evans 2012). On the other hand, in the most heavily obscured SFGs, the ratio of the SFR de- rived from the IR to that derived from e.g. Paα is known to increase with increasing LIR. This trend might arise because in these environments the dust competes for a fraction of the ionizing photons (Alonso-Herrero et al. 2006). Or alterna- tively, that the dust is hotter, increasing the IR output relative to the true SFR (Calzetti e"},{"citing_arxiv_id":"2604.01123","ref_index":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"First results of AMBRA: Abundant Seeds and Early Mergers as a Pathway to the First Massive Black Holes","primary_cat":"astro-ph.GA","submitted_at":"2026-04-01T16:47:19+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Abundant early heavy seeds plus frequent mergers produce the massive black holes seen by JWST at z>9 and yield about four LISA events per year at z>=8.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.20361","ref_index":40,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The HyLight model for hydrogen emission lines in simulated nebulae","primary_cat":"astro-ph.GA","submitted_at":"2025-09-24T17:59:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"HyLight is a new atomic model computing hydrogen recombination line emissivities from local physical conditions, matching Cloudy predictions to within 1% for typical photoionized nebulae.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}