[ { "id": "authors:d0vwm-dmj95", "collection": "authors", "collection_id": "d0vwm-dmj95", "cite_using_url": "https://authors.library.caltech.edu/records/d0vwm-dmj95", "type": "article", "title": "3C 273 host galaxy with Hubble Space Telescope coronagraphy", "author": [ { "family_name": "Ren", "given_name": "Bin B.", "orcid": "0000-0003-1698-9696", "clpid": "Ren-Bin" }, { "family_name": "Fogarty", "given_name": "Kevin", "orcid": "0000-0002-2691-2476", "clpid": "Fogarty-K" }, { "family_name": "Debes", "given_name": "John H.", "orcid": "0000-0002-1783-8817" }, { "family_name": "Meyer", "given_name": "Eileen T.", "orcid": "0000-0002-7676-9962" }, { "family_name": "Mo", "given_name": "Youbin" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Perrin", "given_name": "Marshall D.", "orcid": "0000-0002-3191-8151" }, { "family_name": "Ogle", "given_name": "Patrick M.", "orcid": "0000-0002-3471-981X" }, { "family_name": "Sahlmann", "given_name": "Johannes", "orcid": "0000-0001-9525-3673" } ], "abstract": "

The close-in regions of bright quasars’ host galaxies have been difficult to image due to the overwhelming light coming from quasars. With coronagraphic observations in visible light using the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope, we removed 3C 273 quasar light using color-matching reference stars. The observations revealed the host galaxy from 60″ to 0.″2 with nearly full angular coverage. Isophote modeling has revealed a new core jet, a core blob, and multiple smaller-scale blobs within 2.″5. The blobs could potentially be satellite galaxies or infalling materials towards the central quasar. Using archival STIS data, we constrained the apparent motion of its large scale jets over a 22 yr timeline. By resolving the 3C 273 host galaxy with STIS, our study validates the use of coronagraphs on extragalactic sources for obtaining new insights into the central (at ∼kpc scales) regions of quasar hosts.

", "doi": "10.1051/0004-6361/202348254", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy & Astrophysics", "publication_date": "2024-03", "volume": "683", "pages": "L5" }, { "id": "authors:4gkkn-gw092", "collection": "authors", "collection_id": "4gkkn-gw092", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200123-092045785", "type": "article", "title": "Chandra Observations of the Spectacular A3411\u201312 Merger Event", "author": [ { "family_name": "Andrade-Santos", "given_name": "Felipe", "orcid": "0000-0002-8144-9285", "clpid": "Andrade-Santos-F" }, { "family_name": "van Weeren", "given_name": "Reinout J.", "orcid": "0000-0002-0587-1660", "clpid": "van-Weeren-R-J" }, { "family_name": "Di Gennaro", "given_name": "Gabriella", "orcid": "0000-0002-8648-8507", "clpid": "Di-Gennaro-G" }, { "family_name": "Wittman", "given_name": "David", "orcid": "0000-0002-0813-5888", "clpid": "Wittman-D" }, { "family_name": "Ryu", "given_name": "Dongsu", "orcid": "0000-0002-5455-2957", "clpid": "Ryu-Dongsu" }, { "family_name": "Lal", "given_name": "Dharam Vir", "orcid": "0000-0001-5470-305X", "clpid": "Lal-D-V" }, { "family_name": "Placco", "given_name": "Vinicius M.", "orcid": "0000-0003-4479-1265", "clpid": "Placco-V-M" }, { "family_name": "Fogarty", "given_name": "Kevin", "orcid": "0000-0002-2691-2476", "clpid": "Fogarty-K" }, { "family_name": "Jee", "given_name": "M. James", "clpid": "Jee-M-James" }, { "family_name": "Stroe", "given_name": "Andra", "clpid": "Stroe-A" }, { "family_name": "Sobral", "given_name": "David", "orcid": "0000-0001-8823-4845", "clpid": "Sobral-D" }, { "family_name": "Forman", "given_name": "William R.", "orcid": "0000-0002-9478-1682", "clpid": "Forman-W-R" }, { "family_name": "Jones", "given_name": "Christine", "clpid": "Jones-Christine" }, { "family_name": "Kraft", "given_name": "Ralph P.", "orcid": "0000-0002-0765-0511", "clpid": "Kraft-R-P" }, { "family_name": "Murray", "given_name": "Stephen S.", "clpid": "Murray-S-S" }, { "family_name": "Br\u00fcggen", "given_name": "Marcus", "clpid": "Br\u00fcggen-M" }, { "family_name": "Kang", "given_name": "Hyesung", "orcid": "0000-0002-4674-5687", "clpid": "Kang-Hyesung" }, { "family_name": "Santucci", "given_name": "Rafael", "orcid": "0000-0002-7529-1442", "clpid": "Santucci-R-M" }, { "family_name": "Golovich", "given_name": "Nathan", "orcid": "0000-0003-2632-572X", "clpid": "Golovich-N" }, { "family_name": "Dawson", "given_name": "William", "orcid": "0000-0003-0248-6123", "clpid": "Dawson-W" } ], "abstract": "We present deep Chandra observations of A3411\u201312, a remarkable merging cluster that hosts the most compelling evidence for electron reacceleration at cluster shocks to date. Using the Y_X\u2212M scaling relation, we find r\u2085\u2080\u2080 ~ 1.3 Mpc, M\u2085\u2080\u2080 = (7.1\u00b10.7)\u00d710\u00b9\u2074 M_\u2299, kT = 6.5\u00b10.1 keV, and a gas mass of M_g,\u2085\u2080\u2080 = (9.7\u00b10.1)\u00d710\u00b9\u00b3 M_\u2299. The gas mass fraction within r\u2085\u2080\u2080 is f_g = 0.14\u00b10.01. We compute the shock strength using density jumps to conclude that the Mach number of the merging subcluster is small (M\u2a7d1.15+^(0.14)_(\u22120.09)). We also present density, temperature, pseudo-pressure, and pseudo-entropy maps. Based on the pseudo-entropy map, we conclude that the cluster is undergoing a mild merger, consistent with the small Mach number. On the other hand, radio relics extend over Mpc scale in the A3411\u201312 system, which strongly suggests that a population of energetic electrons already existed over extended regions of the cluster.", "doi": "10.3847/1538-4357/ab4ce5", "issn": "1538-4357", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2019-12-10", "series_number": "1", "volume": "887", "issue": "1", "pages": "Art. No. 31" }, { "id": "authors:vhmpn-6n086", "collection": "authors", "collection_id": "vhmpn-6n086", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190801-085014661", "type": "article", "title": "Dust and Molecular Gas in the Brightest Cluster Galaxy in MACS 1931.8-2635", "author": [ { "family_name": "Fogarty", "given_name": "Kevin", "orcid": "0000-0002-2691-2476", "clpid": "Fogarty-K" }, { "family_name": "Postman", "given_name": "Marc", "orcid": "0000-0002-9365-7989", "clpid": "Postman-Marc" }, { "family_name": "Li", "given_name": "Yuan", "orcid": "0000-0001-5262-6150", "clpid": "Li-Yuan" }, { "family_name": "Dannerbauer", "given_name": "Helmut", "orcid": "0000-0001-7147-3575", "clpid": "Dannerbauer-H" }, { "family_name": "Liu", "given_name": "Hauyu Baobab", "orcid": "0000-0003-2300-2626", "clpid": "Liu-Hauyu-Baobab" }, { "family_name": "Donahue", "given_name": "Megan", "orcid": "0000-0002-2808-0853", "clpid": "Donahue-Megan" }, { "family_name": "Ziegler", "given_name": "Bodo", "clpid": "Ziegler-B" }, { "family_name": "Koekemoer", "given_name": "Anton", "orcid": "0000-0002-6610-2048", "clpid": "Koekemoer-A-M" }, { "family_name": "Frye", "given_name": "Brenda", "clpid": "Frye-Brenda-L" } ], "abstract": "We present new Atacama Large Millimeter Array observations of the molecular gas and far-infrared continuum around the brightest cluster galaxy (BCG) in the cool-core cluster MACS 1931.8-2635. Our observations reveal (1.9 \u00b1 0.3) \u00d7 10^(10) M\u2299 of molecular gas, on par with the largest known reservoirs of cold gas in a cluster core. We detect CO(1\u22120), CO(3\u22122), and CO(4\u22123) emission from both diffuse and compact molecular gas components that extend from the BCG center out to ~30 kpc to the northwest, tracing the UV knots and H\u03b1 filaments observed by the Hubble Space Telescope. Due to the lack of morphological symmetry, we hypothesize that the ~300 km s\u22121 velocity of the CO in the tail is not due to concurrent uplift by active galactic nucleus (AGN) jets; rather, we may be observing the aftermath of a recent AGN outburst. The CO spectral line energy distribution suggests that molecular gas excitation is influenced by processes related to both star formation and recent AGN feedback. Continuum emission in Bands 6 and 7 arises from dust and is spatially coincident with young stars and nebular emission observed in the UV and optical. We constrain the temperature of several dust clumps to be \u227e10 K, which is too cold to be directly interacting with the surrounding ~4.8 keV intracluster medium (ICM). The cold dust population extends beyond the observed CO emission and must either be protected from interacting with the ICM or be surrounded by local volumes of ICM that are several keV colder than observed by Chandra.", "doi": "10.3847/1538-4357/ab22a4", "issn": "1538-4357", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2019-07-10", "series_number": "2", "volume": "879", "issue": "2", "pages": "Art. No. 103" } ]