34,182 results on '"Charlot"'
Search Results
102. Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic Star-Formation Rate Density 300 Myr after the Big Bang
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Robertson, Brant, Johnson, Benjamin D., Tacchella, Sandro, Eisenstein, Daniel J., Hainline, Kevin, Arribas, Santiago, Baker, William M., Bunker, Andrew J., Carniani, Stefano, Carreira, Courtney, Cargile, Phillip A., Charlot, Stéphane, Chevallard, Jacopo, Curti, Mirko, Curtis-Lake, Emma, D'Eugenio, Francesco, Egami, Eiichi, Hausen, Ryan, Helton, Jakob M., Jakobsen, Peter, Ji, Zhiyuan, Jones, Gareth C., Maiolino, Roberto, Maseda, Michael V., Nelson, Erica, Pérez-González, Pablo G., Puskás, Dávid, Rieke, Marcia, Smit, Renske, Sun, Fengwu, Übler, Hannah, Whitler, Lily, Williams, Christina C., Willmer, Christopher N. A., Willott, Chris, and Witstok, Joris
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters spanning $0.4-0.9\mu\mathrm{m}$) and novel JWST images with 14 filters spanning $0.8-5\mu\mathrm{m}$, including 7 medium-band filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data at $>2.3\mu\mathrm{m}$ to construct an ultradeep image, reaching as deep as $\approx31.4$ AB mag in the stack and 30.3-31.0 AB mag ($5\sigma$, $r=0.1"$ circular aperture) in individual filters. We measure photometric redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts $z=11.5-15$. These objects show compact half-light radii of $R_{1/2}\sim50-200$pc, stellar masses of $M_{\star}\sim10^7-10^8 M_{\odot}$, and star-formation rates of $\mathrm{SFR}\sim0.1-1\,M_{\odot}\,\mathrm{yr}^{-1}$. Our search finds no candidates at $15
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- 2023
103. Nebular emission from young stellar populations including binary stars
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Lecroq, M., Charlot, S., Bressan, A., Bruzual, G., Costa, G., Iorio, G., Spera, M., Mapelli, M., Chen, Y., Chevallard, J., and Dall'Amico, M.
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
We investigate the nebular emission produced by young stellar populations using the new GALSEVN model based on the combination of the SEVN population-synthesis code including binary-star processes and the GALAXEV code for the spectral evolution of stellar populations. Photoionization calculations performed with the CLOUDY code confirm that accounting for binary-star processes strongly influences the predicted emission-line properties of young galaxies. In particular, we find that our model naturally reproduces the strong HeII/Hb ratios commonly observed at high Hb equivalent widths in metal-poor, actively star-forming galaxies, which have proven challenging to reproduce using previous models. Including bursty star formation histories broadens the agreement with observations, while the most extreme HeII equivalent widths can be reproduced by models dominated by massive stars. GALSEVN also enables us to compute, for the first time in a way physically consistent with stellar emission, the emission from accretion discs of X-ray binaries (XRBs) and radiative shocks driven by stellar winds and supernova explosions. We find that these contributions are unlikely to prominently affect the predicted HeII/Hb ratio, and that previous claims of a significant contribution by XRBs to the luminosities of high-ionization lines are based on models predicting improbably high ratios of X-ray luminosity to star formation rate, inconsistent with the observed average luminosity function of XRBs in nearby galaxies. The results presented here provide a solid basis for a more comprehensive investigation of the physical properties of observed galaxies with GALSEVN using Bayesian inference., Comment: 26 pages, 18 figures. Accepted for publication in MNRAS
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- 2023
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104. GA-NIFS: JWST discovers an offset AGN 740 million years after the Big Bang
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Übler, Hannah, Maiolino, Roberto, Pérez-González, Pablo G., D'Eugenio, Francesco, Perna, Michele, Curti, Mirko, Arribas, Santiago, Bunker, Andrew, Carniani, Stefano, Charlot, Stéphane, Del Pino, Bruno Rodríguez, Baker, William, Böker, Torsten, Cresci, Giovanni, Dunlop, James, Grogin, Norman A., Jones, Gareth C., Kumari, Nimisha, Lamperti, Isabella, Laporte, Nicolas, Marshall, Madeline A., Mazzolari, Giovanni, Parlanti, Eleonora, Rawle, Tim, Scholtz, Jan, Venturi, Giacomo, and Witstok, Joris
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Astrophysics - Astrophysics of Galaxies - Abstract
A surprising finding of recent studies is the large number of Active Galactic Nuclei (AGN) associated with moderately massive black holes ($\rm \log(M_\bullet/M_\odot)\sim 6-8$), in the first billion years after the Big Bang ($z>5$). In this context, a relevant finding has been the large fraction of candidate dual AGN, both at large separations (several kpc) and in close pairs (less than a kpc), likely in the process of merging. Frequent black hole merging may be a route for black hole growth in the early Universe; however, previous findings are still tentative and indirect. We present JWST/NIRSpec-IFU observations of a galaxy at $z=7.15$ in which we find evidence for a $\rm \log(M_\bullet/M_\odot)\sim7.7$ accreting black hole, as traced by a broad component of H$\beta$ emission, associated with the Broad Line Region (BLR) around the black hole. This BLR is offset by 620 pc in projection from the centroid of strong rest-frame optical emission, with a velocity offset of $\sim$40 km/s. The latter region is also characterized by (narrow) nebular emission features typical of AGN, hence also likely hosting another accreting black hole, although obscured (type 2, narrow-line AGN). We exclude that the offset BLR is associated with Supernovae or massive stars, and we interpret these results as two black holes in the process of merging. This finding may be relevant for estimates of the rate and properties of gravitational wave signals from the early Universe that will be detected by future observatories like LISA., Comment: 12 pages, 5 figures; accepted for publication in MNRAS; doi:10.1093/mnras/stae943
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- 2023
105. GA-NIFS: The core of an extremely massive proto-cluster at the Epoch of Reionization probed with JWST/NIRSpec
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Arribas, Santiago, Perna, Michele, Del Pino, Bruno Rodríguez, Lamperti, Isabella, D'Eugenio, Francesco, Pérez-González, Pablo G., Jones, Gareth C., Crespo, Alejandro, Curti, Mirko, Lim, Seunghwan, Álvarez-Márquez, Javier, Bunker, Andrew J., Carniani, Stefano, Charlot, Stéphane, Jakobsen, Peter, Maiolino, Roberto, Übler, Hannah, Willott, Chris J., Böker, Torsten, Chevallard, Jacopo, Circosta, Chiara, Cresci, Giovanni, Kumari, Nimisha, Parlanti, Eleonora, Scholtz, Jan, Venturi, Giacomo, and Witstok, Joris
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Astrophysics - Astrophysics of Galaxies - Abstract
The SPT0311-58 system resides in a massive dark matter halo at z ~ 6.9. It hosts two dusty galaxies (E and W) with a combined star formation rate of ~3500 Msun/yr. Its surrounding field exhibits an overdensity of sub-mm sources, making it a candidate proto-cluster. We use spatially-resolved spectroscopy provided by the JWST/NIRSpec Integral Field Unit (IFU) to probe a field of view (FoV) ~ 17 x 17 kpc^2 around this object. These observations have revealed ten new galaxies at z ~ 6.9, characterised by dynamical masses spanning from ~10^9 to 10^10 Msun and a range in radial velocities of ~ 1500 km/s, in addition to the already known E and W galaxies. The implied large number density, and the wide spread in velocities, indicate that SPT0311-58 is at the core of a proto-cluster, immersed in a very massive dark matter halo of ~ 5 x 10^12 Msun. Hence, it represents the most massive proto-cluster ever found at the EoR. We also study the dynamical stage of the system and find that it likely is not fully virialised. The galaxies exhibit a great diversity of properties showing a range of evolutionary stages. We derive their ongoing Ha-based unobscured SFR, and find that its contribution to the total SF varies significantly across the galaxies in the system. Their ionization conditions range from those typical of field galaxies at similar redshift recently studied with JWST to those found in more evolved objects at lower z. The metallicity spans more than 0.8 dex across the FoV, reaching nearly solar values in some cases. The detailed IFU spectroscopy of the E galaxy reveals that it is actively assembling its stellar mass, showing sub-kpc inhomogeneities, and a metallicity gradient that can be explained by accretion of low metallicity gas from the IGM. The kinematic maps indicate departures from regular rotation, high turbulence, and a possible pre-collision minor merger. (Abridged), Comment: Revised version: minor changes, improved figures, updated references
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- 2023
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106. Measurement of inclusive and differential cross sections of single top quark production in association with a W boson in proton-proton collisions at s = 13.6 TeV
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Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Hussain, P. S., Jeitler, M., Krammer, N., Li, A., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Waltenberger, W., Wulz, C.-E., Janssen, T., Van Laer, T., Van Mechelen, P., Breugelmans, N., D’Hondt, J., Dansana, S., De Moor, A., Delcourt, M., Heyen, F., Lowette, S., Makarenko, I., Müller, D., Tavernier, S., Tytgat, M., Van Onsem, G. P., Van Putte, S., Vannerom, D., Bilin, B., Clerbaux, B., Das, A. K., De Lentdecker, G., Evard, H., Favart, L., Gianneios, P., Jaramillo, J., Khalilzadeh, A., Khan, F. A., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Shahzad, M. A., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., De Coen, M., Dobur, D., Gokbulut, G., Hong, Y., Knolle, J., Lambrecht, L., Marckx, D., Mota Amarilo, K., Skovpen, K., Van Den Bossche, N., van der Linden, J., Wezenbeek, L., Benecke, A., Bethani, A., Bruno, G., Caputo, C., De Favereau De Jeneret, J., Delaere, C., Donertas, I. S., Giammanco, A., Guzel, A. O., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Tran, T. T., Wertz, S., Alves, G. A., Alves Gallo Pereira, M., Coelho, E., Correia Silva, G., Hensel, C., Menezes De Oliveira, T., Mora Herrera, C., Moraes, A., Rebello Teles, P., Soeiro, M., Vilela Pereira, A., Aldá Júnior, W. L., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., Fonseca De Souza, S., Gomes De Souza, R., Laux Kuhn, T., Macedo, M., Martins, J., Mundim, L., Nogima, H., Pinheiro, J. P., Santoro, A., Sznajder, A., Thiel, M., Bernardes, C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gregores, E. M., Maietto Silverio, I., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Laroze, D., Thakur, S., Cheng, T., Javaid, T., Yuan, L., Hu, Z., Liang, Z., Liu, J., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Sharma, R., Song, J. N., Tao, J., Wang, C., Wang, J., Wang, Z., Zhang, H., Zhao, J., Agapitos, A., Ban, Y., Deng, S., Guo, B., Jiang, C., Levin, A., Li, C., Li, Q., Mao, Y., Qian, S., Qian, S. J., Qin, X., Sun, X., Wang, D., Yang, H., Zhang, L., Zhao, Y., Zhou, C., Yang, S., You, Z., Jaffel, K., Lu, N., Bauer, G., Li, B., Yi, K., Zhang, J., Gao, X., Li, Y., Lin, Z., Lu, C., Xiao, M., Avila, C., Barbosa Trujillo, D. A., Cabrera, A., Florez, C., Fraga, J., Reyes Vega, J. A., Ramirez, F., Rendón, C., Rodriguez, M., Ruales Barbosa, A. A., Ruiz Alvarez, J. D., Giljanovic, D., Godinovic, N., Lelas, D., Sculac, A., Kovac, M., Petkovic, A., Sculac, T., Bargassa, P., Brigljevic, V., Chitroda, B. K., Ferencek, D., Jakovcic, K., Starodumov, A., Susa, T., Attikis, A., Christoforou, K., Hadjiagapiou, A., Leonidou, C., Mousa, J., Nicolaou, C., Paizanos, L., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka, H., Stepennov, A., Finger, M., Finger, Jr., M., Kveton, A., Carrera Jarrin, E., Abdalla, H., Abu Zeid, S., Assran, Y., Abdullah Al-Mashad, M., Mahmoud, M. A., Ehataht, K., Kadastik, M., Lange, T., Nandan, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken, C., Kirschenmann, H., Osterberg, K., Voutilainen, M., Bharthuar, S., Bin Norjoharuddeen, N., Brücken, E., Garcia, F., Inkaew, P., Kallonen, K. T. S., Lampén, T., Lassila-Perini, K., Lehti, S., Lindén, T., Myllymäki, M., Rantanen, M. m., Siikonen, H., Tuominiemi, J., Luukka, P., Petrow, H., Besancon, M., Couderc, F., Dejardin, M., Denegri, D., Faure, J. L., Ferri, F., Ganjour, S., Gras, P., Hamel de Monchenault, G., Kumar, M., Lohezic, V., Malcles, J., Orlandi, F., Portales, L., Rosowsky, A., Sahin, M. Ö., Savoy-Navarro, A., Simkina, P., Titov, M., Tornago, M., Beaudette, F., Boldrini, G., Busson, P., Cappati, A., Charlot, C., Chiusi, M., Damas, F., Davignon, O., De Wit, A., Ehle, I. T., Fontana Santos Alves, B. A., Ghosh, S., Gilbert, A., Granier de Cassagnac, R., Hakimi, A., Harikrishnan, B., Kalipoliti, L., Liu, G., Nguyen, M., Ochando, C., Salerno, R., Sauvan, J. B., Sirois, Y., Urda Gómez, L., Vernazza, E., Zabi, A., Zghiche, A., Agram, J.-L., Andrea, J., Apparu, D., Bloch, D., Brom, J.-M., Chabert, E. C., Collard, C., Falke, S., Goerlach, U., Haeberle, R., Le Bihan, A.-C., Meena, M., Poncet, O., Saha, G., Sessini, M. A., Van Hove, P., Vaucelle, P., Di Florio, A., Amram, D., Beauceron, S., Blancon, B., Boudoul, G., Chanon, N., Contardo, D., Depasse, P., Dozen, C., El Mamouni, H., Fay, J., Gascon, S., Gouzevitch, M., Greenberg, C., Grenier, G., Ille, B., Jourd‘huy, E., Laktineh, I. B., Lethuillier, M., Mirabito, L., Perries, S., Purohit, A., Vander Donckt, M., Verdier, P., Xiao, J., Lomidze, I., Toriashvili, T., Tsamalaidze, Z., Botta, V., Consuegra Rodríguez, S., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Pérez Adán, D., Röwert, N., Teroerde, M., Diekmann, S., Dodonova, A., Eich, N., Eliseev, D., Engelke, F., Erdmann, J., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Jung, A., Lee, M. y., Mausolf, F., Merschmeyer, M., Meyer, A., Mukherjee, S., Noll, D., Nowotny, F., Pozdnyakov, A., Rath, Y., Redjeb, W., Rehm, F., Reithler, H., Sarkisovi, V., Schmidt, A., Seth, C., Sharma, A., Spah, J. L., Stein, A., Torres Da Silva De Araujo, F., Wiedenbeck, S., Zaleski, S., Dziwok, C., Flügge, G., Kress, T., Nowack, A., Pooth, O., Stahl, A., Ziemons, T., Zotz, A., Aarup Petersen, H., Aldaya Martin, M., Alimena, J., Amoroso, S., An, Y., Bach, J., Baxter, S., Bayatmakou, M., Becerril Gonzalez, H., Behnke, O., Belvedere, A., Blekman, F., Borras, K., Campbell, A., Cardini, A., Cheng, C., Colombina, F., Eckerlin, G., Eckstein, D., Estevez Banos, L. I., Filatov, O., Gallo, E., Geiser, A., Guglielmi, V., Guthoff, M., Hinzmann, A., Jeppe, L., Kaech, B., Kasemann, M., Kleinwort, C., Kogler, R., Komm, M., Krücker, D., Lange, W., Leyva Pernia, D., Lipka, K., Lohmann, W., Lorkowski, F., Mankel, R., Melzer-Pellmann, I.-A., Mendizabal Morentin, M., Meyer, A. B., Milella, G., Moral Figueroa, K., Mussgiller, A., Nair, L. P., Niedziela, J., Nürnberg, A., Otarid, Y., Park, J., Ranken, E., Raspereza, A., Rastorguev, D., Rübenach, J., Rygaard, L., Saggio, A., Scham, M., Schnake, S., Schütze, P., Schwanenberger, C., Selivanova, D., Sharko, K., Shchedrolosiev, M., Stafford, D., Vazzoler, F., Ventura Barroso, A., Walsh, R., Wang, D., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Yang, Y., Zimermmane Castro Santos, A., Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bollweg, S., Bonanomi, M., Connor, P., El Morabit, K., Fischer, Y., Garutti, E., Grohsjean, A., Haller, J., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kuo, C. c., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Pena Rodriguez, K. J., Quadfasel, T., Raciti, B., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Elicabuk, U., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Hofsaess, R., Horzela, M., Husemann, U., Kieseler, J., Klute, M., Koppenhöfer, R., Lawhorn, J. M., Link, M., Lintuluoto, A., Maier, S., Mitra, S., Mormile, M., Müller, Th., Neukum, M., Oh, M., Pfeffer, E., Presilla, M., Quast, G., Rabbertz, K., Regnery, B., Shadskiy, N., Shvetsov, I., Simonis, H. J., Sowa, L., Stockmeier, L., Tauqeer, K., Toms, M., Trevisani, N., Von Cube, R. F., Wassmer, M., Wieland, S., Wittig, F., Wolf, R., Zuo, X., Anagnostou, G., Daskalakis, G., Kyriakis, A., Papadopoulos, A., Stakia, A., Kontaxakis, P., Melachroinos, G., Painesis, Z., Papavergou, I., Paraskevas, I., Saoulidou, N., Theofilatos, K., Tziaferi, E., Vellidis, K., Zisopoulos, I., Bakas, G., Chatzistavrou, T., Karapostoli, G., Kousouris, K., Papakrivopoulos, I., Siamarkou, E., Tsipolitis, G., Zacharopoulou, A., Adamidis, K., Bestintzanos, I., Evangelou, I., Foudas, C., Kamtsikis, C., Katsoulis, P., Kokkas, P., Kosmoglou Kioseoglou, P. G., Manthos, N., Papadopoulos, I., Strologas, J., Hajdu, C., Horvath, D., Márton, K., Rádl, A. J., Sikler, F., Veszpremi, V., Csanád, M., Farkas, K., Fehérkuti, A., Gadallah, M. M. A., Kadlecsik, Á., Major, P., Pásztor, G., Veres, G. I., Olah, L., Ujvari, B., Bencze, G., Czellar, S., Molnar, J., Szillasi, Z., Nemes, F., Novak, T., Bansal, S., Beri, S. B., Bhatnagar, V., Chaudhary, G., Chauhan, S., Dhingra, N., Kaur, A., Kaur, A., Kaur, H., Kaur, M., Kumar, S., Sheokand, T., Singh, J. B., Singla, A., Ahmed, A., Bhardwaj, A., Chhetri, A., Choudhary, B. C., Kumar, A., Kumar, A., Naimuddin, M., Ranjan, K., Saini, M. K., Saumya, S., Baradia, S., Barman, S., Bhattacharya, S., Das Gupta, S., Dutta, S., Dutta, S., Sarkar, S., Ameen, M. M., Behera, P. K., Behera, S. C., Chatterjee, S., Dash, G., Jana, P., Kalbhor, P., Kamble, S., Komaragiri, J. R., Kumar, D., Mishra, T., Parida, B., Pujahari, P. R., Saha, N. R., Sharma, A., Sikdar, A. K., Singh, R. K., Verma, P., Verma, S., Vijay, A., Dugad, S., Mohanty, G. B., Shelake, M., Suryadevara, P., Bala, A., Banerjee, S., Chatterjee, R. M., Guchait, M., Jain, Sh., Jaiswal, A., Kumar, S., Majumder, G., Mazumdar, K., Parolia, S., Thachayath, A., Bahinipati, S., Kar, C., Maity, D., Mal, P., Muraleedharan Nair Bindhu, V. K., Naskar, K., Nayak, A., Nayak, S., Pal, K., Sadangi, P., Swain, S. K., Varghese, S., Vats, D., Acharya, S., Alpana, A., Dube, S., Gomber, B., Hazarika, P., Kansal, B., Laha, A., Sahu, B., Sharma, S., Vaish, K. Y., Bakhshiansohi, H., Jafari, A., Zeinali, M., Bashiri, S., Chenarani, S., Etesami, S. M., Hosseini, Y., Khakzad, M., Khazaie, E., Mohammadi Najafabadi, M., Tizchang, S., Felcini, M., Grunewald, M., Abbrescia, M., Colaleo, A., Creanza, D., D’Anzi, B., De Filippis, N., De Palma, M., Elmetenawee, W., Fiore, L., Iaselli, G., Longo, L., Louka, M., Maggi, G., Maggi, M., Margjeka, I., Mastrapasqua, V., My, S., Nuzzo, S., Pellecchia, A., Pompili, A., Pugliese, G., Radogna, R., Ramos, D., Ranieri, A., Silvestris, L., Simone, F. M., Sözbilir, Ü., Stamerra, A., Troiano, D., Venditti, R., Verwilligen, P., Zaza, A., Abbiendi, G., Battilana, C., Bonacorsi, D., Capiluppi, P., Castro, A., Cavallo, F. R., Cuffiani, M., Dallavalle, G. M., Diotalevi, T., Fabbri, F., Fanfani, A., Fasanella, D., Giacomelli, P., Giommi, L., Grandi, C., Guiducci, L., Lo Meo, S., Lorusso, M., Lunerti, L., Marcellini, S., Masetti, G., Navarria, F. L., Paggi, G., Perrotta, A., Primavera, F., Rossi, A. M., Rossi Tisbeni, S., Rovelli, T., Siroli, G. P., Costa, S., Di Mattia, A., Lapertosa, A., Potenza, R., Tricomi, A., Tuve, C., Assiouras, P., Barbagli, G., Bardelli, G., Camaiani, B., Cassese, A., Ceccarelli, R., Ciulli, V., Civinini, C., D’Alessandro, R., Focardi, E., Kello, T., Latino, G., Lenzi, P., Lizzo, M., Meschini, M., Paoletti, S., Papanastassiou, A., Sguazzoni, G., Viliani, L., Benussi, L., Bianco, S., Meola, S., Piccolo, D., Chatagnon, P., Ferro, F., Robutti, E., Tosi, S., Benaglia, A., Brivio, F., Cetorelli, F., De Guio, F., Dinardo, M. E., Dini, P., Gennai, S., Gerosa, R., Ghezzi, A., Govoni, P., Guzzi, L., Lucchini, M. T., Malberti, M., Malvezzi, S., Massironi, A., Menasce, D., Moroni, L., Paganoni, M., Palluotto, S., Pedrini, D., Perego, A., Pinolini, B. S., Pizzati, G., Ragazzi, S., Tabarelli de Fatis, T., Buontempo, S., Cagnotta, A., Carnevali, F., Cavallo, N., Fabozzi, F., Iorio, A. O. M., Lista, L., Paolucci, P., Rossi, B., Ardino, R., Azzi, P., Bacchetta, N., Bortignon, P., Bortolato, G., Bragagnolo, A., Bulla, A. C. M., Carlin, R., Checchia, P., Dorigo, T., Gasparini, F., Gasparini, U., Giorgetti, S., Lusiani, E., Margoni, M., Meneguzzo, A. T., Michelotto, M., Migliorini, M., Pazzini, J., Ronchese, P., Rossin, R., Simonetto, F., Tosi, M., Triossi, A., Ventura, S., Zanetti, M., Zotto, P., Zucchetta, A., Zumerle, G., Braghieri, A., Calzaferri, S., Fiorina, D., Montagna, P., Re, V., Riccardi, C., Salvini, P., Vai, I., Vitulo, P., Ajmal, S., Ascioti, M. E., Bilei, G. 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W., Hurtado Anampa, K., Ivanov, T., Jessop, C., Lannon, K., Lawrence, J., Loukas, N., Lutton, L., Mariano, J., Marinelli, N., Mcalister, I., McCauley, T., Mcgrady, C., Moore, C., Musienko, Y., Nelson, H., Osherson, M., Piccinelli, A., Ruchti, R., Townsend, A., Wan, Y., Wayne, M., Yockey, H., Zarucki, M., Zygala, L., Basnet, A., Carrigan, M., Durkin, L. S., Hill, C., Joyce, M., Nunez Ornelas, M., Wei, K., Winer, B. L., Yates, B. R., Bouchamaoui, H., Coldham, K., Das, P., Dezoort, G., Elmer, P., Frankenthal, A., Greenberg, B., Haubrich, N., Kennedy, K., Kopp, G., Kwan, S., Lange, D., Loeliger, A., Marlow, D., Ojalvo, I., Olsen, J., Stickland, D., Tully, C., Malik, S., Bakshi, A. S., Chandra, S., Chawla, R., Gu, A., Gutay, L., Jones, M., Jung, A. W., Koshy, A. M., Liu, M., Negro, G., Neumeister, N., Paspalaki, G., Piperov, S., Scheurer, V., Schulte, J. F., Stojanovic, M., Thieman, J., Virdi, A. K., Wang, F., Wildridge, A., Xie, W., Yao, Y., Dolen, J., Parashar, N., Pathak, A., Acosta, D., Carnahan, T., Ecklund, K. M., Fernández Manteca, P. J., Freed, S., Gardner, P., Geurts, F. J. M., Krommydas, I., Li, W., Lin, J., Miguel Colin, O., Padley, B. P., Redjimi, R., Rotter, J., Yigitbasi, E., Zhang, Y., Bodek, A., de Barbaro, P., Demina, R., Dulemba, J. L., Garcia-Bellido, A., Hindrichs, O., Khukhunaishvili, A., Parmar, N., Parygin, P., Taus, R., Chiarito, B., Chou, J. P., Clark, S. V., Gadkari, D., Gershtein, Y., Halkiadakis, E., Heindl, M., Houghton, C., Jaroslawski, D., Konstantinou, S., Laflotte, I., Lath, A., Montalvo, R., Nash, K., Reichert, J., Routray, H., Saha, P., Salur, S., Schnetzer, S., Somalwar, S., Stone, R., Thayil, S. A., Thomas, S., Vora, J., Wang, H., Ally, D., Delannoy, A. G., Fiorendi, S., Higginbotham, S., Holmes, T., Kanuganti, A. R., Karunarathna, N., Lee, L., Nibigira, E., Spanier, S., Aebi, D., Ahmad, M., Akhter, T., Androsov, K., Bouhali, O., Eusebi, R., Gilmore, J., Huang, T., Kamon, T., Kim, H., Luo, S., Mueller, R., Overton, D., Rathjens, D., Safonov, A., Akchurin, N., Damgov, J., Gogate, N., Hegde, V., Hussain, A., Kazhykarim, Y., Lamichhane, K., Lee, S. W., Mankel, A., Peltola, T., Volobouev, I., Appelt, E., Chen, Y., Greene, S., Gurrola, A., Johns, W., Kunnawalkam Elayavalli, R., Melo, A., Romeo, F., Sheldon, P., Tuo, S., Velkovska, J., Viinikainen, J., Cardwell, B., Chung, H., Cox, B., Hakala, J., Hirosky, R., Ledovskoy, A., Neu, C., Bhattacharya, S., Karchin, P. E., Aravind, A., Banerjee, S., Black, K., Bose, T., Chavez, E., Dasu, S., De Bruyn, I., Everaerts, P., Galloni, C., He, H., Herndon, M., Herve, A., Koraka, C. K., Lanaro, A., Loveless, R., Madhusudanan Sreekala, J., Mallampalli, A., Mohammadi, A., Mondal, S., Parida, G., Pétré, L., Pinna, D., Savin, A., Shang, V., Sharma, V., Smith, W. 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- 2025
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107. Measurement of the double-differential inclusive jet cross section in proton-proton collisions at s = 5.02 TeV
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Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Escalante Del Valle, A., Hussain, P. S., Jeitler, M., Krammer, N., Lechner, L., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Templ, S., Waltenberger, W., Wulz, C.-E., Darwish, M. R., Janssen, T., Kello, T., Van Mechelen, P., Bols, E. S., D’Hondt, J., De Moor, A., Delcourt, M., El Faham, H., Lowette, S., Makarenko, I., Morton, A., Müller, D., Sahasransu, A. R., Tavernier, S., Van Putte, S., Vannerom, D., Clerbaux, B., Dansana, S., De Lentdecker, G., Favart, L., Hohov, D., Jaramillo, J., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Pétré, L., Postiau, N., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., De Coen, M., Dobur, D., Knolle, J., Lambrecht, L., Mestdach, G., Rendón, C., Samalan, A., Skovpen, K., Tytgat, M., Van Den Bossche, N., Vermassen, B., Wezenbeek, L., Benecke, A., Bruno, G., Bury, F., Caputo, C., Delaere, C., Donertas, I. S., Giammanco, A., Jaffel, K., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Mondal, K., Tran, T. T., Vischia, P., Wertz, S., Alves, G. A., Coelho, E., Hensel, C., Moraes, A., Rebello Teles, P., Aldá Júnior, W. L., Alves Gallo Pereira, M., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., Dos Santos Sousa, V., Fonseca De Souza, S., Martins, J., Mora Herrera, C., Mota Amarilo, K., Mundim, L., Nogima, H., Santoro, A., Silva Do Amaral, S. M., Sznajder, A., Thiel, M., Vilela Pereira, A., Bernardes, C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gregores, E. M., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Ivanov, T., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Thakur, S., Cheng, T., Guo, Q., Javaid, T., Mittal, M., Yuan, L., Bauer, G., Hu, Z., Lezki, S., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Monti, F., Sharma, R., Song, J. N., Tao, J., Wang, J., Zhang, H., Agapitos, A., Ban, Y., Levin, A., Li, C., Li, Q., Lyu, X., Mao, Y., Qian, S. J., Sun, X., Wang, D., Yang, H., Lu, M., You, Z., Lu, N., Gao, X., Leggat, D., Okawa, H., Zhang, Y., Lin, Z., Lu, C., Xiao, M., Avila, C., Barbosa Trujillo, D. A., Cabrera, A., Florez, C., Fraga, J., Reyes Vega, J. A., Mejia Guisao, J., Ramirez, F., Rodriguez, M., Ruiz Alvarez, J. D., Giljanovic, D., Godinovic, N., Lelas, D., Sculac, A., Kovac, M., Sculac, T., Bargassa, P., Brigljevic, V., Chitroda, B. K., Ferencek, D., Mishra, S., Starodumov, A., Susa, T., Attikis, A., Christoforou, K., Konstantinou, S., Mousa, J., Nicolaou, C., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka, H., Stepennov, A., Finger, M., Finger, Jr., M., Kveton, A., Ayala, E., Carrera Jarrin, E., Elgammal, S., Ellithi Kamel, A., Mahmoud, M. A., Mohammed, Y., Ehataht, K., Kadastik, M., Lange, T., Nandan, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken, C., Kirschenmann, H., Osterberg, K., Voutilainen, M., Bharthuar, S., Brücken, E., Garcia, F., Havukainen, J., Kim, M. S., Kinnunen, R., Lampén, T., Lassila-Perini, K., Lehti, S., Lindén, T., Lotti, M., Martikainen, L., Myllymäki, M., Rantanen, M. m., Siikonen, H., Tuominen, E., Tuominiemi, J., Luukka, P., Petrow, H., Tuuva, T., Amendola, C., Besancon, M., Couderc, F., Dejardin, M., Denegri, D., Faure, J. L., Ferri, F., Ganjour, S., Gras, P., Hamel de Monchenault, G., Lohezic, V., Malcles, J., Rander, J., Rosowsky, A., Sahin, M. Ö., Savoy-Navarro, A., Simkina, P., Titov, M., Baldenegro Barrera, C., Beaudette, F., Buchot Perraguin, A., Busson, P., Cappati, A., Charlot, C., Damas, F., Davignon, O., Diab, B., Falmagne, G., Fontana Santos Alves, B. A., Ghosh, S., Granier de Cassagnac, R., Hakimi, A., Harikrishnan, B., Liu, G., Motta, J., Nguyen, M., Ochando, C., Portales, L., Salerno, R., Sarkar, U., Sauvan, J. B., Sirois, Y., Tarabini, A., Vernazza, E., Zabi, A., Zghiche, A., Agram, J.-L., Andrea, J., Apparu, D., Bloch, D., Brom, J.-M., Chabert, E. 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C., Sharma, A., Stein, A., Torres Da Silva De Araujo, F., Vigilante, L., Wiedenbeck, S., Zaleski, S., Dziwok, C., Flügge, G., Haj Ahmad, W., Kress, T., Nowack, A., Pooth, O., Stahl, A., Ziemons, T., Zotz, A., Aarup Petersen, H., Aldaya Martin, M., Alimena, J., Amoroso, S., An, Y., Baxter, S., Bayatmakou, M., Becerril Gonzalez, H., Behnke, O., Bhattacharya, S., Blekman, F., Borras, K., Brunner, D., Campbell, A., Cardini, A., Cheng, C., Colombina, F., Consuegra Rodríguez, S., Correia Silva, G., De Silva, M., Eckerlin, G., Eckstein, D., Estevez Banos, L. I., Filatov, O., Gallo, E., Geiser, A., Giraldi, A., Greau, G., Grohsjean, A., Guglielmi, V., Guthoff, M., Jafari, A., Jomhari, N. Z., Kaech, B., Kasemann, M., Kaveh, H., Kleinwort, C., Kogler, R., Komm, M., Krücker, D., Lange, W., Leyva Pernia, D., Lipka, K., Lohmann, W., Mankel, R., Melzer-Pellmann, I.-A., Mendizabal Morentin, M., Metwally, J., Meyer, A. B., Milella, G., Mormile, M., Mussgiller, A., Nürnberg, A., Otarid, Y., Pérez Adán, D., Ranken, E., Raspereza, A., Ribeiro Lopes, B., Rübenach, J., Saggio, A., Scham, M., Scheurer, V., Schnake, S., Schütze, P., Schwanenberger, C., Shchedrolosiev, M., Sosa Ricardo, R. E., Sreelatha Pramod, L. P., Stafford, D., Vazzoler, F., Ventura Barroso, A., Walsh, R., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Wuchterl, S., Yang, Y., Zimermmane Castro Santos, A., Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bonanomi, M., Connor, P., De Leo, K., Eich, M., El Morabit, K., Fröhlich, A., Garbers, C., Garutti, E., Hajheidari, M., Haller, J., Hinzmann, A., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Mehta, A., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Pena Rodriguez, K. J., Quadfasel, T., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Horzela, M., Husemann, U., Klute, M., Koppenhöfer, R., Link, M., Lintuluoto, A., Maier, S., Mitra, S., Müller, Th., Neukum, M., Quast, G., Rabbertz, K., Shvetsov, I., Simonis, H. 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G., Fiorendi, S., Holmes, T., Karunarathna, N., Lee, L., Nibigira, E., Spanier, S., Ahmad, M., Bouhali, O., Dalchenko, M., Delgado, A., Eusebi, R., Gilmore, J., Huang, T., Kamon, T., Kim, H., Luo, S., Malhotra, S., Mueller, R., Overton, D., Rathjens, D., Safonov, A., Akchurin, N., Damgov, J., Hegde, V., Lamichhane, K., Lee, S. W., Mengke, T., Muthumuni, S., Peltola, T., Volobouev, I., Whitbeck, A., Appelt, E., Greene, S., Gurrola, A., Johns, W., Kunnawalkam Elayavalli, R., Melo, A., Romeo, F., Sheldon, P., Tuo, S., Velkovska, J., Viinikainen, J., Cardwell, B., Cox, B., Hakala, J., Hirosky, R., Ledovskoy, A., Li, A., Neu, C., Perez Lara, C. E., Karchin, P. E., Aravind, A., Banerjee, S., Black, K., Bose, T., Dasu, S., De Bruyn, I., Everaerts, P., Galloni, C., He, H., Herndon, M., Herve, A., Koraka, C. K., Lanaro, A., Loveless, R., Madhusudanan Sreekala, J., Mallampalli, A., Mohammadi, A., Mondal, S., Parida, G., Pinna, D., Savin, A., Shang, V., Sharma, V., Smith, W. 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S., Zarubin, A., Zhizhin, I., and Zhokin, A.
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- 2025
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108. Model-independent search for pair production of new bosons decaying into muons in proton-proton collisions at s = 13 TeV
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Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Hussain, P. S., Jeitler, M., Krammer, N., Li, A., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Templ, S., Waltenberger, W., Wulz, C.-E., Darwish, M. R., Janssen, T., Van Laer, T., Van Mechelen, P., Breugelmans, N., D’Hondt, J., Dansana, S., De Moor, A., Delcourt, M., Heyen, F., Lowette, S., Makarenko, I., Müller, D., Tavernier, S., Tytgat, M., Van Onsem, G. P., Van Putte, S., Vannerom, D., Bilin, B., Clerbaux, B., Das, A. K., De Lentdecker, G., Evard, H., Favart, L., Gianneios, P., Jaramillo, J., Khalilzadeh, A., Khan, F. A., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Shahzad, M. A., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., De Coen, M., Dobur, D., Gokbulut, G., Hong, Y., Knolle, J., Lambrecht, L., Marckx, D., Mota Amarilo, K., Samalan, A., Skovpen, K., Van Den Bossche, N., van der Linden, J., Wezenbeek, L., Benecke, A., Bethani, A., Bruno, G., Caputo, C., De Favereau De Jeneret, J., Delaere, C., Donertas, I. S., Giammanco, A., Guzel, A. O., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Tran, T. T., Wertz, S., Alves, G. A., Alves Gallo Pereira, M., Coelho, E., Correia Silva, G., Hensel, C., Menezes De Oliveira, T., Mora Herrera, C., Moraes, A., Rebello Teles, P., Soeiro, M., Vilela Pereira, A., Aldá Júnior, W. L., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., Fonseca De Souza, S., Gomes De Souza, R., Macedo, M., Martins, J., Mundim, L., Nogima, H., Pinheiro, J. P., Santoro, A., Sznajder, A., Thiel, M., Bernardes, C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gregores, E. M., Lopes Da Costa, B., Maietto Silverio, I., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Thakur, S., Cheng, T., Javaid, T., Yuan, L., Hu, Z., Liang, Z., Liu, J., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Sharma, R., Song, J. N., Tao, J., Wang, C., Wang, J., Wang, Z., Zhang, H., Zhao, J., Agapitos, A., Ban, Y., Deng, S., Guo, B., Jiang, C., Levin, A., Li, C., Li, Q., Mao, Y., Qian, S., Qian, S. J., Qin, X., Sun, X., Wang, D., Yang, H., Zhang, L., Zhao, Y., Zhou, C., Yang, S., You, Z., Jaffel, K., Lu, N., Bauer, G., Li, B., Zhang, J., Gao, X., Lin, Z., Lu, C., Xiao, M., Avila, C., Barbosa Trujillo, D. A., Cabrera, A., Florez, C., Fraga, J., Reyes Vega, J. A., Ramirez, F., Rendón, C., Rodriguez, M., Ruales Barbosa, A. A., Ruiz Alvarez, J. D., Giljanovic, D., Godinovic, N., Lelas, D., Sculac, A., Kovac, M., Petkovic, A., Sculac, T., Bargassa, P., Brigljevic, V., Chitroda, B. K., Ferencek, D., Jakovcic, K., Mishra, S., Starodumov, A., Susa, T., Attikis, A., Christoforou, K., Hadjiagapiou, A., Leonidou, C., Mousa, J., Nicolaou, C., Paizanos, L., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka, H., Stepennov, A., Finger, M., Finger, Jr., M., Kveton, A., Carrera Jarrin, E., Assran, Y., El-mahdy, B., Elgammal, S., Lotfy, A., Mohammed, Y., Ehataht, K., Kadastik, M., Lange, T., Nandan, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken, C., Kirschenmann, H., Osterberg, K., Voutilainen, M., Bharthuar, S., Bin Norjoharuddeen, N., Brücken, E., Garcia, F., Inkaew, P., Kallonen, K. T. 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C., Collard, C., Falke, S., Goerlach, U., Haeberle, R., Le Bihan, A.-C., Meena, M., Poncet, O., Saha, G., Sessini, M. A., Van Hove, P., Vaucelle, P., Di Florio, A., Amram, D., Beauceron, S., Blancon, B., Boudoul, G., Chanon, N., Contardo, D., Depasse, P., Dozen, C., El Mamouni, H., Fay, J., Gascon, S., Gouzevitch, M., Greenberg, C., Grenier, G., Ille, B., Jourd’huy, E., Laktineh, I. B., Lethuillier, M., Mirabito, L., Perries, S., Purohit, A., Vander Donckt, M., Verdier, P., Xiao, J., Bagaturia, I., Lomidze, I., Tsamalaidze, Z., Botta, V., Consuegra Rodríguez, S., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Pérez Adán, D., Röwert, N., Teroerde, M., Diekmann, S., Dodonova, A., Eich, N., Eliseev, D., Engelke, F., Erdmann, J., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Jung, A., Lee, M. y., Mausolf, F., Merschmeyer, M., Meyer, A., Mukherjee, S., Noll, D., Nowotny, F., Pozdnyakov, A., Rath, Y., Redjeb, W., Rehm, F., Reithler, H., Sarkisovi, V., Schmidt, A., Sharma, A., Spah, J. L., Stein, A., Torres Da Silva De Araujo, F., Wiedenbeck, S., Zaleski, S., Dziwok, C., Flügge, G., Kress, T., Nowack, A., Pooth, O., Stahl, A., Ziemons, T., Zotz, A., Aarup Petersen, H., Aldaya Martin, M., Alimena, J., Amoroso, S., An, Y., Bach, J., Baxter, S., Bayatmakou, M., Becerril Gonzalez, H., Behnke, O., Belvedere, A., Bhattacharya, S., Blekman, F., Borras, K., Campbell, A., Cardini, A., Cheng, C., Colombina, F., De Silva, M., Eckerlin, G., Eckstein, D., Estevez Banos, L. I., Filatov, O., Gallo, E., Geiser, A., Guglielmi, V., Guthoff, M., Hinzmann, A., Jeppe, L., Kaech, B., Kasemann, M., Kleinwort, C., Kogler, R., Komm, M., Krücker, D., Lange, W., Leyva Pernia, D., Lipka, K., Lohmann, W., Lorkowski, F., Mankel, R., Melzer-Pellmann, I.-A., Mendizabal Morentin, M., Meyer, A. B., Milella, G., Moral Figueroa, K., Mussgiller, A., Nair, L. P., Niedziela, J., Nürnberg, A., Otarid, Y., Park, J., Ranken, E., Raspereza, A., Rastorguev, D., Rübenach, J., Rygaard, L., Saggio, A., Scham, M., Schnake, S., Schütze, P., Schwanenberger, C., Selivanova, D., Sharko, K., Shchedrolosiev, M., Stafford, D., Vazzoler, F., Ventura Barroso, A., Walsh, R., Wang, D., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Yang, Y., Zimermmane Castro Santos, A., Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bollweg, S., Bonanomi, M., Connor, P., El Morabit, K., Fischer, Y., Garutti, E., Grohsjean, A., Haller, J., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kuo, C. c., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Pena Rodriguez, K. J., Quadfasel, T., Raciti, B., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Hofsaess, R., Horzela, M., Husemann, U., Kieseler, J., Klute, M., Koppenhöfer, R., Lawhorn, J. M., Link, M., Lintuluoto, A., Maier, B., Maier, S., Mitra, S., Mormile, M., Müller, Th., Neukum, M., Oh, M., Pfeffer, E., Presilla, M., Quast, G., Rabbertz, K., Regnery, B., Shadskiy, N., Shvetsov, I., Simonis, H. J., Sowa, L., Stockmeier, L., Tauqeer, K., Toms, M., Trevisani, N., Von Cube, R. 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K., Varghese, S., Vats, D., Acharya, S., Alpana, A., Dube, S., Gomber, B., Hazarika, P., Kansal, B., Laha, A., Sahu, B., Sharma, S., Vaish, K. Y., Bakhshiansohi, H., Jafari, A., Zeinali, M., Bashiri, S., Chenarani, S., Etesami, S. M., Hosseini, Y., Khakzad, M., Khazaie, E., Mohammadi Najafabadi, M., Tizchang, S., Felcini, M., Grunewald, M., Abbrescia, M., Colaleo, A., Creanza, D., D’Anzi, B., De Filippis, N., De Palma, M., Elmetenawee, W., Fiore, L., Iaselli, G., Longo, L., Louka, M., Maggi, G., Maggi, M., Margjeka, I., Mastrapasqua, V., My, S., Nuzzo, S., Pellecchia, A., Pompili, A., Pugliese, G., Radogna, R., Ramos, D., Ranieri, A., Silvestris, L., Simone, F. M., Sözbilir, Ü., Stamerra, A., Troiano, D., Venditti, R., Verwilligen, P., Zaza, A., Abbiendi, G., Battilana, C., Bonacorsi, D., Capiluppi, P., Castro, A., Cavallo, F. R., Cuffiani, M., Dallavalle, G. 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W., Hurtado Anampa, K., Ivanov, T., Jessop, C., Lannon, K., Lawrence, J., Loukas, N., Lutton, L., Mariano, J., Marinelli, N., Mcalister, I., McCauley, T., Mcgrady, C., Moore, C., Musienko, Y., Nelson, H., Osherson, M., Piccinelli, A., Ruchti, R., Townsend, A., Wan, Y., Wayne, M., Yockey, H., Zarucki, M., Zygala, L., Basnet, A., Bylsma, B., Carrigan, M., Durkin, L. S., Hill, C., Joyce, M., Nunez Ornelas, M., Wei, K., Winer, B. L., Yates, B. R., Bouchamaoui, H., Das, P., Dezoort, G., Elmer, P., Frankenthal, A., Greenberg, B., Haubrich, N., Kennedy, K., Kopp, G., Kwan, S., Lange, D., Loeliger, A., Marlow, D., Ojalvo, I., Olsen, J., Shevelev, A., Stickland, D., Tully, C., Malik, S., Bakshi, A. S., Chandra, S., Chawla, R., Gu, A., Gutay, L., Jones, M., Jung, A. W., Koshy, A. M., Liu, M., Negro, G., Neumeister, N., Paspalaki, G., Piperov, S., Scheurer, V., Schulte, J. F., Stojanovic, M., Thieman, J., Virdi, A. 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R., Karunarathna, N., Lee, L., Nibigira, E., Spanier, S., Aebi, D., Ahmad, M., Akhter, T., Bouhali, O., Eusebi, R., Gilmore, J., Huang, T., Kamon, T., Kim, H., Luo, S., Mueller, R., Overton, D., Rathjens, D., Safonov, A., Akchurin, N., Damgov, J., Gogate, N., Hegde, V., Hussain, A., Kazhykarim, Y., Lamichhane, K., Lee, S. W., Mankel, A., Peltola, T., Volobouev, I., Appelt, E., Chen, Y., Greene, S., Gurrola, A., Johns, W., Kunnawalkam Elayavalli, R., Melo, A., Romeo, F., Sheldon, P., Tuo, S., Velkovska, J., Viinikainen, J., Cardwell, B., Cox, B., Hakala, J., Hirosky, R., Ledovskoy, A., Neu, C., Bhattacharya, S., Karchin, P. E., Aravind, A., Banerjee, S., Black, K., Bose, T., Dasu, S., De Bruyn, I., Everaerts, P., Galloni, C., He, H., Herndon, M., Herve, A., Koraka, C. K., Lanaro, A., Loveless, R., Madhusudanan Sreekala, J., Mallampalli, A., Mohammadi, A., Mondal, S., Parida, G., Pétré, L., Pinna, D., Savin, A., Shang, V., Sharma, V., Smith, W. H., Teague, D., Tsoi, H. F., Vetens, W., Warden, A., Afanasiev, S., Alexakhin, V., Budkouski, D., Golutvin, I., Gorbunov, I., Karjavine, V., Korenkov, V., Lanev, A., Malakhov, A., Matveev, V., Palichik, V., Perelygin, V., Savina, M., Shalaev, V., Shmatov, S., Shulha, S., Smirnov, V., Teryaev, O., Voytishin, N., Yuldashev, B. S., Zarubin, A., Zhizhin, I., Gavrilov, G., Golovtcov, V., Ivanov, Y., Kim, V., Levchenko, P., Murzin, V., Oreshkin, V., Sosnov, D., Sulimov, V., Uvarov, L., Vorobyev, A., Andreev, Yu., Dermenev, A., Gninenko, S., Golubev, N., Karneyeu, A., Kirpichnikov, D., Kirsanov, M., Krasnikov, N., Tlisova, I., Toropin, A., Aushev, T., Gavrilov, V., Lychkovskaya, N., Nikitenko, A., Popov, V., Zhokin, A., Chadeeva, M., Chistov, R., Polikarpov, S., Andreev, V., Azarkin, M., Kirakosyan, M., Terkulov, A., Boos, E., Bunichev, V., Dubinin, M., Dudko, L., Gribushin, A., Klyukhin, V., Kodolova, O., Obraztsov, S., Perfilov, M., Petrushanko, S., Savrin, V., Vorotnikov, G., Blinov, V., Dimova, T., Kozyrev, A., Radchenko, O., Skovpen, Y., Kachanov, V., Konstantinov, D., Slabospitskii, S., Uzunian, A., Babaev, A., Borshch, V., Druzhkin, D., Chekhovsky, V., and Makarenko, V.
- Published
- 2024
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109. Measurement of boosted Higgs bosons produced via vector boson fusion or gluon fusion in the H →bb¯s decay mode using LHC proton-proton collision data at bb¯s = 13 TeV
- Author
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Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Hussain, P. S., Jeitler, M., Krammer, N., Li, A., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Templ, S., Waltenberger, W., Wulz, C.-E., Darwish, M. R., Janssen, T., Van Mechelen, P., Bols, E. S., D’Hondt, J., Dansana, S., De Moor, A., Delcourt, M., El Faham, H., Lowette, S., Makarenko, I., Müller, D., Tavernier, S., Tytgat, M., Van Onsem, G. P., Van Putte, S., Vannerom, D., Clerbaux, B., Das, A. K., De Lentdecker, G., Evard, H., Favart, L., Gianneios, P., Hohov, D., Jaramillo, J., Khalilzadeh, A., Khan, F. A., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., De Coen, M., Dobur, D., Hong, Y., Knolle, J., Lambrecht, L., Mestdach, G., Mota Amarilo, K., Rendón, C., Samalan, A., Skovpen, K., Van Den Bossche, N., van der Linden, J., Wezenbeek, L., Benecke, A., Bethani, A., Bruno, G., Caputo, C., Delaere, C., Donertas, I. S., Giammanco, A., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Mondal, K., Tran, T. T., Wertz, S., Alves, G. A., Coelho, E., Hensel, C., Menezes De Oliveira, T., Moraes, A., Rebello Teles, P., Soeiro, M., Aldá Júnior, W. L., Alves Gallo Pereira, M., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., Fonseca De Souza, S., Gomes De Souza, R., Martins, J., Mora Herrera, C., Mundim, L., Nogima, H., Pinheiro, J. P., Santoro, A., Sznajder, A., Thiel, M., Vilela Pereira, A., Bernardes, C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gregores, E. M., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Thakur, S., Cheng, T., Javaid, T., Yuan, L., Hu, Z., Liu, J., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Sharma, R., Song, J. N., Tao, J., Wang, C., Wang, J., Wang, Z., Zhang, H., Agapitos, A., Ban, Y., Levin, A., Li, C., Li, Q., Mao, Y., Qian, S. J., Sun, X., Wang, D., Yang, H., Zhang, L., Zhou, C., You, Z., Jaffel, K., Lu, N., Bauer, G., Gao, X., Leggat, D., Okawa, H., Lin, Z., Lu, C., Xiao, M., Avila, C., Barbosa Trujillo, D. A., Cabrera, A., Florez, C., Fraga, J., Reyes Vega, J. A., Mejia Guisao, J., Ramirez, F., Rodriguez, M., Ruiz Alvarez, J. D., Giljanovic, D., Godinovic, N., Lelas, D., Sculac, A., Kovac, M., Sculac, T., Bargassa, P., Brigljevic, V., Chitroda, B. K., Ferencek, D., Jakovcic, K., Mishra, S., Starodumov, A., Susa, T., Attikis, A., Christoforou, K., Konstantinou, S., Mousa, J., Nicolaou, C., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka, H., Stepennov, A., Finger, M., Finger, Jr., M., Kveton, A., Ayala, E., Carrera Jarrin, E., Abdelalim, A. A., Salama, E., Abdullah Al-Mashad, M., Mahmoud, M. A., Ehataht, K., Kadastik, M., Lange, T., Nandan, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken, C., Kirschenmann, H., Osterberg, K., Voutilainen, M., Bharthuar, S., Brücken, E., Garcia, F., Kallonen, K. T. S., Kinnunen, R., Lampén, T., Lassila-Perini, K., Lehti, S., Lindén, T., Martikainen, L., Myllymäki, M., Rantanen, M. m., Siikonen, H., Tuominen, E., Tuominiemi, J., Luukka, P., Petrow, H., Besancon, M., Couderc, F., Dejardin, M., Denegri, D., Faure, J. L., Ferri, F., Ganjour, S., Gras, P., Hamel de Monchenault, G., Lohezic, V., Malcles, J., Rander, J., Rosowsky, A., Sahin, M. Ö., Savoy-Navarro, A., Simkina, P., Titov, M., Tornago, M., Baldenegro Barrera, C., Beaudette, F., Buchot Perraguin, A., Busson, P., Cappati, A., Charlot, C., Chiusi, M., Damas, F., Davignon, O., De Wit, A., Fontana Santos Alves, B. A., Ghosh, S., Gilbert, A., Granier de Cassagnac, R., Hakimi, A., Harikrishnan, B., Kalipoliti, L., Liu, G., Motta, J., Nguyen, M., Ochando, C., Portales, L., Salerno, R., Sauvan, J. B., Sirois, Y., Tarabini, A., Vernazza, E., Zabi, A., Zghiche, A., Agram, J.-L., Andrea, J., Apparu, D., Bloch, D., Brom, J.-M., Chabert, E. C., Collard, C., Falke, S., Goerlach, U., Grimault, C., Haeberle, R., Le Bihan, A.-C., Meena, M., Saha, G., Sessini, M. A., Van Hove, P., Beauceron, S., Blancon, B., Boudoul, G., Chanon, N., Choi, J., Contardo, D., Depasse, P., Dozen, C., El Mamouni, H., Fay, J., Gascon, S., Gouzevitch, M., Greenberg, C., Grenier, G., Ille, B., Laktineh, I. B., Lethuillier, M., Mirabito, L., Perries, S., Purohit, A., Vander Donckt, M., Verdier, P., Xiao, J., Adamov, G., Lomidze, I., Tsamalaidze, Z., Botta, V., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Röwert, N., Teroerde, M., Diekmann, S., Dodonova, A., Eich, N., Eliseev, D., Engelke, F., Erdmann, J., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Jung, A., Lee, M. y., Mausolf, F., Merschmeyer, M., Meyer, A., Mukherjee, S., Noll, D., Nowotny, F., Pozdnyakov, A., Rath, Y., Redjeb, W., Rehm, F., Reithler, H., Sarkar, U., Sarkisovi, V., Schmidt, A., Sharma, A., Spah, J. L., Stein, A., Torres Da Silva De Araujo, F., Vigilante, L., Wiedenbeck, S., Zaleski, S., Dziwok, C., Flügge, G., Haj Ahmad, W., Kress, T., Nowack, A., Pooth, O., Stahl, A., Ziemons, T., Zotz, A., Aarup Petersen, H., Aldaya Martin, M., Alimena, J., Amoroso, S., An, Y., Baxter, S., Bayatmakou, M., Becerril Gonzalez, H., Behnke, O., Belvedere, A., Bhattacharya, S., Blekman, F., Borras, K., Campbell, A., Cardini, A., Cheng, C., Colombina, F., Consuegra Rodríguez, S., Correia Silva, G., De Silva, M., Eckerlin, G., Eckstein, D., Estevez Banos, L. I., Filatov, O., Gallo, E., Geiser, A., Giraldi, A., Guglielmi, V., Guthoff, M., Hinzmann, A., Jafari, A., Jeppe, L., Jomhari, N. Z., Kaech, B., Kasemann, M., Kleinwort, C., Kogler, R., Komm, M., Krücker, D., Lange, W., Leyva Pernia, D., Lipka, K., Lohmann, W., Mankel, R., Melzer-Pellmann, I.-A., Mendizabal Morentin, M., Meyer, A. B., Milella, G., Mussgiller, A., Nair, L. P., Nürnberg, A., Otarid, Y., Park, J., Pérez Adán, D., Ranken, E., Raspereza, A., Ribeiro Lopes, B., Rübenach, J., Saggio, A., Scham, M., Schnake, S., Schütze, P., Schwanenberger, C., Selivanova, D., Sharko, K., Shchedrolosiev, M., Sosa Ricardo, R. E., Stafford, D., Vazzoler, F., Ventura Barroso, A., Walsh, R., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Yang, Y., Zimermmane Castro Santos, A., Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bollweg, S., Bonanomi, M., Connor, P., Eich, M., El Morabit, K., Fischer, Y., Garbers, C., Garutti, E., Grohsjean, A., Haller, J., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Mehta, A., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Pena Rodriguez, K. J., Quadfasel, T., Raciti, B., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Hofsaess, R., Horzela, M., Husemann, U., Kieseler, J., Klute, M., Koppenhöfer, R., Lawhorn, J. M., Link, M., Lintuluoto, A., Maier, S., Mitra, S., Mormile, M., Müller, Th., Neukum, M., Oh, M., Pfeffer, E., Presilla, M., Quast, G., Rabbertz, K., Regnery, B., Shadskiy, N., Shvetsov, I., Simonis, H. J., Toms, M., Trevisani, N., Von Cube, R. 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E., Aravind, A., Banerjee, S., Black, K., Bose, T., Dasu, S., De Bruyn, I., Everaerts, P., Galloni, C., He, H., Herndon, M., Herve, A., Koraka, C. K., Lanaro, A., Loveless, R., Madhusudanan Sreekala, J., Mallampalli, A., Mohammadi, A., Mondal, S., Parida, G., Pétré, L., Pinna, D., Savin, A., Shang, V., Sharma, V., Smith, W. H., Teague, D., Tsoi, H. F., Vetens, W., Warden, A., Afanasiev, S., Budkouski, D., Golutvin, I., Gorbunov, I., Karjavine, V., Korenkov, V., Lanev, A., Malakhov, A., Matveev, V., Palichik, V., Perelygin, V., Savina, M., Shalaev, V., Shmatov, S., Shulha, S., Smirnov, V., Teryaev, O., Voytishin, N., Yuldashev, B. 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110. Portable Acceleration of CMS Computing Workflows with Coprocessors as a Service
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Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Hussain, P. S., Jeitler, M., Krammer, N., Li, A., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Templ, S., Waltenberger, W., Wulz, C.-E., Darwish, M. R., Janssen, T., Mechelen, P. Van, Bols, E. S., D’Hondt, J., Dansana, S., De Moor, A., Delcourt, M., Faham, H. El, Lowette, S., Makarenko, I., Müller, D., Sahasransu, A. R., Tavernier, S., Tytgat, M., Onsem, G. P. Van, Putte, S. Van, Vannerom, D., Clerbaux, B., Das, A. K., De Lentdecker, G., Favart, L., Gianneios, P., Hohov, D., Jaramillo, J., Khalilzadeh, A., Khan, F. A., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Thomas, L., Bemden, M. Vanden, Velde, C. Vander, Vanlaer, P., De Coen, M., Dobur, D., Hong, Y., Knolle, J., Lambrecht, L., Mestdach, G., Amarilo, K. Mota, Rendón, C., Samalan, A., Skovpen, K., Bossche, N. Van Den, Linden, J. van der, Wezenbeek, L., Benecke, A., Bethani, A., Bruno, G., Caputo, C., Delaere, C., Donertas, I. S., Giammanco, A., Jaffel, K., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Mondal, K., Tran, T. T., Wertz, S., Alves, G. A., Coelho, E., Hensel, C., De Oliveira, T. Menezes, Moraes, A., Teles, P. Rebello, Soeiro, M., Júnior, W. L. Aldá, Pereira, M. Alves Gallo, Filho, M. Barroso Ferreira, Malbouisson, H. Brandao, Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., De Souza, S. Fonseca, De Souza, R. Gomes, Martins, J., Herrera, C. Mora, Mundim, L., Nogima, H., Pinheiro, J. P., Santoro, A., Sznajder, A., Thiel, M., Pereira, A. Vilela, Bernardes, C. A., Calligaris, L., Tomei, T. R. Fernandez Perez, Gregores, E. M., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Thakur, S., Cheng, T., Javaid, T., Yuan, L., Hu, Z., Liu, J., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Sharma, R., Song, J. N., Tao, J., Wang, C., Wang, J., Wang, Z., Zhang, H., Agapitos, A., Ban, Y., Levin, A., Li, C., Li, Q., Mao, Y., Qian, S. J., Sun, X., Wang, D., Yang, H., Zhang, L., Zhou, C., You, Z., Lu, N., Bauer, G., Gao, X., Leggat, D., Okawa, H., Lin, Z., Lu, C., Xiao, M., Avila, C., Trujillo, D. A. Barbosa, Cabrera, A., Florez, C., Fraga, J., Vega, J. A. Reyes, Guisao, J. Mejia, Ramirez, F., Rodriguez, M., Alvarez, J. D. Ruiz, Giljanovic, D., Godinovic, N., Lelas, D., Sculac, A., Kovac, M., Sculac, T., Bargassa, P., Brigljevic, V., Chitroda, B. 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Ventura, Walsh, R., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Yang, Y., Santos, A. Zimermmane Castro, Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bollweg, S., Bonanomi, M., Connor, P., Eich, M., Morabit, K. El, Fischer, Y., Garbers, C., Garutti, E., Grohsjean, A., Haller, J., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Mehta, A., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Rodriguez, K. J. Pena, Quadfasel, T., Raciti, B., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Hofsaess, R., Horzela, M., Husemann, U., Kieseler, J., Klute, M., Koppenhöfer, R., Lawhorn, J. M., Link, M., Lintuluoto, A., Maier, S., Mitra, S., Mormile, M., Müller, Th., Neukum, M., Oh, M., Presilla, M., Quast, G., Rabbertz, K., Regnery, B., Shadskiy, N., Shvetsov, I., Simonis, H. J., Toms, M., Trevisani, N., Cube, R. F. Von, Wassmer, M., Wieland, S., Wittig, F., Wolf, R., Zuo, X., Anagnostou, G., Daskalakis, G., Kyriakis, A., Papadopoulos, A., Stakia, A., Kontaxakis, P., Melachroinos, G., Panagiotou, A., Papavergou, I., Paraskevas, I., Saoulidou, N., Theofilatos, K., Tziaferi, E., Vellidis, K., Zisopoulos, I., Bakas, G., Chatzistavrou, T., Karapostoli, G., Kousouris, K., Papakrivopoulos, I., Siamarkou, E., Tsipolitis, G., Zacharopoulou, A., Adamidis, K., Bestintzanos, I., Evangelou, I., Foudas, C., Kamtsikis, C., Katsoulis, P., Kokkas, P., Kioseoglou, P. G. Kosmoglou, Manthos, N., Papadopoulos, I., Strologas, J., Bartók, M., Hajdu, C., Horvath, D., Márton, K., Sikler, F., Veszpremi, V., Csanád, M., Farkas, K., Gadallah, M. M. A., Kadlecsik, Á., Major, P., Mandal, K., Pásztor, G., Rádl, A. J., Veres, G. I., Raics, P., Ujvari, B., Zilizi, G., Bencze, G., Czellar, S., Molnar, J., Szillasi, Z., Csorgo, T., Nemes, F., Novak, T., Babbar, J., Bansal, S., Beri, S. B., Bhatnagar, V., Chaudhary, G., Chauhan, S., Dhingra, N., Kaur, A., Kaur, A., Kaur, H., Kaur, M., Kumar, S., Sandeep, K., Sheokand, T., Singh, J. B., Singla, A., Ahmed, A., Bhardwaj, A., Chhetri, A., Choudhary, B. C., Kumar, A., Kumar, A., Naimuddin, M., Ranjan, K., Saumya, S., Baradia, S., Barman, S., Bhattacharya, S., Dutta, S., Dutta, S., Sarkar, S., Ameen, M. M., Behera, P. K., Behera, S. C., Chatterjee, S., Jana, P., Kalbhor, P., Komaragiri, J. R., Kumar, D., Pujahari, P. R., Saha, N. R., Sharma, A., Sikdar, A. K., Verma, S., Dugad, S., Kumar, M., Mohanty, G. B., Suryadevara, P., Bala, A., Banerjee, S., Chatterjee, R. M., Dewanjee, R. 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K., Wang, F., Xie, W., Dolen, J., Parashar, N., Pathak, A., Acosta, D., Carnahan, T., Ecklund, K. M., Manteca, P. J. Fernández, Freed, S., Gardner, P., Geurts, F. J. M., Li, W., Colin, O. Miguel, Padley, B. P., Redjimi, R., Rotter, J., Yigitbasi, E., Zhang, Y., Bodek, A., de Barbaro, P., Demina, R., Dulemba, J. L., Garcia-Bellido, A., Hindrichs, O., Khukhunaishvili, A., Parmar, N., Parygin, P., Popova, E., Taus, R., Goulianos, K., Chiarito, B., Chou, J. P., Gershtein, Y., Halkiadakis, E., Heindl, M., Houghton, C., Jaroslawski, D., Karacheban, O., Laflotte, I., Lath, A., Montalvo, R., Nash, K., Routray, H., Salur, S., Schnetzer, S., Somalwar, S., Stone, R., Thayil, S. A., Thomas, S., Vora, J., Wang, H., Acharya, H., Ally, D., Delannoy, A. G., Fiorendi, S., Higginbotham, S., Holmes, T., Kanuganti, A. R., Karunarathna, N., Lee, L., Nibigira, E., Spanier, S., Aebi, D., Ahmad, M., Bouhali, O., Eusebi, R., Gilmore, J., Huang, T., Kamon, T., Kim, H., Luo, S., Mueller, R., Overton, D., Rathjens, D., Safonov, A., Akchurin, N., Damgov, J., Hegde, V., Hussain, A., Kazhykarim, Y., Lamichhane, K., Lee, S. W., Mankel, A., Peltola, T., Volobouev, I., Whitbeck, A., Appelt, E., Chen, Y., Greene, S., Gurrola, A., Johns, W., Elayavalli, R. Kunnawalkam, Melo, A., Romeo, F., Sheldon, P., Tuo, S., Velkovska, J., Viinikainen, J., Cardwell, B., Cox, B., Hakala, J., Hirosky, R., Ledovskoy, A., Neu, C., Lara, C. E. Perez, Karchin, P. E., Aravind, A., Banerjee, S., Black, K., Bose, T., Dasu, S., De Bruyn, I., Everaerts, P., Galloni, C., He, H., Herndon, M., Herve, A., Koraka, C. K., Lanaro, A., Loveless, R., Sreekala, J. Madhusudanan, Mallampalli, A., Mohammadi, A., Mondal, S., Parida, G., Pétré, L., Pinna, D., Savin, A., Shang, V., Sharma, V., Smith, W. H., Teague, D., Tsoi, H. F., Vetens, W., Warden, A., Afanasiev, S., Andreev, V., Andreev, Yu., Aushev, T., Azarkin, M., Babaev, A., Belyaev, A., Blinov, V., Boos, E., Borshch, V., Budkouski, D., Chadeeva, M., Chekhovsky, V., Chistov, R., Demiyanov, A., Dermenev, A., Dimova, T., Druzhkin, D., Dubinin, M., Dudko, L., Ershov, A., Gavrilov, G., Gavrilov, V., Gninenko, S., Golovtcov, V., Golubev, N., Golutvin, I., Gorbunov, I., Gribushin, A., Ivanov, Y., Kachanov, V., Karjavine, V., Karneyeu, A., Kim, V., Kirakosyan, M., Kirpichnikov, D., Kirsanov, M., Klyukhin, V., Kodolova, O., Korenkov, V., Kozyrev, A., Krasnikov, N., Lanev, A., Levchenko, P., Lychkovskaya, N., Makarenko, V., Malakhov, A., Matveev, V., Murzin, V., Nikitenko, A., Obraztsov, S., Oreshkin, V., Palichik, V., Perelygin, V., Petrushanko, S., Polikarpov, S., Popov, V., Radchenko, O., Savina, M., Savrin, V., Shalaev, V., Shmatov, S., Shulha, S., Skovpen, Y., Slabospitskii, S., Smirnov, V., Snigirev, A., Sosnov, D., Sulimov, V., Tcherniaev, E., Terkulov, A., Teryaev, O., Tlisova, I., Toropin, A., Uvarov, L., Uzunian, A., Vorobyev, A., Voytishin, N., Yuldashev, B. S., Zarubin, A., Zhizhin, I., and Zhokin, A.
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111. “The least significant change on bone mineral density scan increased in patients with higher degrees of obesity”
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Dorilleau, Claire, Kanagaratnam, Lukshe, Charlot, Isabelle, Hittinger , Ambre, Bertin, Eric, Salmon, Jean-Hugues, and Geoffroy, Marion
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- 2024
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112. Correction: Endometriosis MR mimickers: T2-hypointense lesions
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Ruaux, Edouard, VanBuren, Wendaline M., Nougaret, Stéphanie, Gavrel, Marie, Charlot, Mathilde, Grangeon, Flavia, Bolze, Pierre-Adrien, Thomassin-Naggara, Isabelle, and Rousset, Pascal
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- 2024
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113. Formation and evolution of secondary phases and surface altered layers during borosilicate glass corrosion in pore water
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Wang, Kaifeng, Chen, Yang, Findling, Nathaniel, Charlot, Frederic, Charlet, Laurent, Liu, Jiliang, and Zhang, Zhentao
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- 2024
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114. Endometriosis MR mimickers: T2-hypointense lesions
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Ruaux, Edouard, VanBuren, Wendaline M., Nougaret, Stéphanie, Gavrel, Marie, Charlot, Mathilde, Grangeon, Flavia, Bolze, Pierre-Adrien, Thomassin-Naggara, Isabelle, and Rousset, Pascal
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- 2024
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115. JADES: A large population of obscured, narrow line AGN at high redshift
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Scholtz, Jan, Maiolino, Roberto, D'Eugenio, Francesco, Curtis-Lake, Emma, Carniani, Stefano, Charlot, Stephane, Curti, Mirko, Silcock, Maddie S., Arribas, Santiago, Baker, William, Bhatawdekar, Rachana, Boyett, Kristan, Bunker, Andrew J., Chevallard, Jacopo, Circosta, Chiara, Eisenstein, Daniel J., Hainline, Kevin, Hausen, Ryan, Ji, Xihan, Ji, Zhiyuan, Johnson, Benjamin D., Kumari, Nimisha, Looser, Tobias J., Lyu, Jianwei, Maseda, Michael V., Parlanti, Eleonora, Perna, Michele, Rieke, Marcia, Robertson, Brant, Del Pino, Bruno Rodríguez, Sun, Fengwu, Tacchella, Sandro, Übler, Hannah, Venturi, Giacomo, Williams, Christina C., Willmer, Christopher N. A., Willott, Chris, and Witstok, Joris
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Astrophysics - Astrophysics of Galaxies - Abstract
We present the identification of 42 narrow-line active galactic nuclei (type-2 AGN) candidates in the two deepest observations of the JADES spectroscopic survey with JWST/NIRSpec. The spectral coverage and the depth of our observations allow us to select narrow-line AGNs based on both rest-frame optical and UV emission lines up to z=10. Due to the metallicity decrease of galaxies, at $z>3$ the standard optical diagnostic diagrams (N2-BPT or S2-VO87) become unable to distinguish many AGN from other sources of photoionisation. Therefore, we also use high ionisation lines, such as HeII$\lambda$4686, HeII$\lambda$1640, NeIV$\lambda$2422, NeV$\lambda$3420, and NV$\lambda$1240, also in combination with other UV transitions, to trace the presence of AGN. Out of a parent sample of 209 galaxies, we identify 42 type-2 AGN (although 10 of them are tentative), giving a fraction of galaxies in JADES hosting type-2 AGN of about $20\pm3$\%, which does not evolve significantly in the redshift range between 2 and 10. The selected type-2 AGN have estimated bolometric luminosities of $10^{41.3-44.9}$ erg s$^{-1}$ and host-galaxy stellar masses of $10^{7.2-9.3}$ M$_{\odot}$. The star formation rates of the selected AGN host galaxies are consistent with those of the star-forming main sequence. The AGN host galaxies at z=4-6 contribute $\sim$8-30 \% to the UV luminosity function, slightly increasing with UV luminosity., Comment: 23 pages 13 figures
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- 2023
116. JWST spectroscopy of $z\sim 5-8$ UV-selected galaxies: New constraints on the evolution of the Ly$\alpha$ escape fraction in the reionization era
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Chen, Zuyi, Stark, Daniel P., Mason, Charlotte, Topping, Michael W., Whitler, Lily, Tang, Mengtao, Endsley, Ryan, and Charlot, Stéphane
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Astrophysics - Astrophysics of Galaxies - Abstract
We describe {\it JWST}/NIRSpec prism measurements of Ly$\alpha$ emission in $z\gtrsim 5$ galaxies. We identify Ly$\alpha$ detections in 10 out of 69 galaxies with robust rest-optical emission line redshift measurements at $5\leq z<7$ in the CEERS and DDT-2750 observations of the EGS field. Galaxies at $z\simeq 6$ with faint continuum (F150W $=$ 27--29 mag) are found with extremely large rest-frame Ly$\alpha$ equivalent widths (ranging up to 286 A). Likely Ly$\alpha$ detections are also seen in two new $z>7$ galaxies ($z=$ 7.49 and 7.17) from the second epoch of CEERS observations, both showing large Ly$\alpha$ equivalent widths that likely indicate significant transmission through the IGM. We measure high Ly$\alpha$ escape fractions in the 12 Ly$\alpha$ emitters in our sample (median 0.28), two of which show $f_{\rm esc}^{ {\rm Ly}\alpha}$ near unity ($>0.80$). We find that $50_{-11}^{+11}$% of $z\simeq 6$ galaxies with [OIII]+H$\beta$ EW $>$ 1000 A have $f_{\rm esc}^{ {\rm Ly}\alpha}$ $>0.2$, consistent with the fractions found in lower-redshift samples with matched [OIII]+H$\beta$ EWs. While uncertainties are still significant, we find that only $10_{-5}^{+9}$% of $z>7$ galaxies with similarly strong rest optical emission lines show such large $f_{\rm esc}^{ {\rm Ly}\alpha}$, as may be expected if IGM attenuation of Ly$\alpha$ increases towards higher redshifts. We identify photometric galaxy overdensities near the $z\gtrsim 7$ Ly$\alpha$ emitters, potentially providing the ionizing flux necessary to create large ionized sightlines that facilitate Ly$\alpha$ transmission. Finally, we investigate the absence of Ly$\alpha$ emission in a comparable (and spectroscopically confirmed) galaxy overdensity at $z=7.88$ in the Abell 2744 field, discussing new prism spectra of the field obtained with the UNCOVER program., Comment: main text 20 pages, 13 figures; accepted for publication by MNRAS
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- 2023
117. Variation of the stellar initial mass function in semi-analytical models III: testing the cosmic ray regulated integrated galaxy-wide initial mass function
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Fontanot, Fabio, La Barbera, Francesco, De Lucia, Gabriella, Cecchi, Rachele, Xie, Lizhi, Hirschmann, Michaela, Bruzual, Gustavo, Charlot, Stéphane, and Vazdekis, Alexandre
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Astrophysics - Astrophysics of Galaxies - Abstract
In our previous work, we derive the CR-IGIMF: a new scenario for a variable stellar initial mass function (IMF), which combines numerical results on the role played by cosmic rays in setting the thermal state of star forming gas, with the analytical approach of the integrated galaxy-wide IMF. In this work, we study the implications of this scenario for the properties of local Early-Type galaxies (ETG), as inferred from dynamical, photometric and spectroscopic studies. We implement a library of CR-IGIMF shapes in the framework of the Galaxy Evolution and Assembly (GAEA) model. Our realization includes a derivation of synthetic spectral energy distribution for each model galaxy, allowing a direct derivation of the mass fraction in the mean IMF of low-mass stars (i.e. the dwarf-to-giant ratio - $\rm f_{dg}$) and a comparison with IMF sensitive spectral features. The predictions of the GAEA model implementing the CR-IGIMF confirm our previous findings: it correctly reproduces both the observed excess of z$\sim$0 dynamical mass (mass-to-light ratios) with respect to spectroscopic (photometric) estimates assuming a universal, MW-like, IMF, and the observed increase of [$\alpha$/Fe] ratios with stellar mass in spheroidal galaxies. Moreover, this realization reproduces the increasing trends of $\rm f_{dg}$, and IMF-sensitive line-strengths with velocity dispersion, although the predicted relations are significantly shallower than the observed ones. Our results show that the CR-IGIMF is a promising scenario that reproduces at the same time dynamical, photometric and spectroscopic indications of a varying IMF in local ETGs. The shallow relations found for spectral indices suggest that either a stronger variability as a function of galaxy properties or additional dependences (e.g. as a function of star forming gas metallicity) might be required to match the strength of the observed trends., Comment: 13 pages, 8 figures, 2 tables, A&A accepted
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- 2023
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118. JADES: Carbon enrichment 350 Myr after the Big Bang in a gas-rich galaxy
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D'Eugenio, Francesco, Maiolino, Roberto, Carniani, Stefano, Curtis-Lake, Emma, Witstok, Joris, Chevallard, Jacopo, Charlot, Stephane, Baker, William M., Arribas, Santiago, Boyett, Kristan, Bunker, Andrew J., Curti, Mirko, Eisenstein, Daniel J., Hainline, Kevin, Ji, Zhiyuan, Johnson, Benjamin D., Looser, Tobias J., Nakajima, Kimihiko, Nelson, Erica, Rieke, Marcia, Robertson, Brant, Scholtz, Jan, Smit, Renske, Venturi, Giacomo, Tacchella, Sandro, Uebler, Hannah, Willmer, Christopher N. A., and Willott, Chris
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Astrophysics - Astrophysics of Galaxies - Abstract
Finding the emergence of the first generation of metals in the early Universe, and identifying their origin, are some of the most important goals of modern astrophysics. We present deep JWST/NIRSpec spectroscopy of GS-z12, a galaxy at z=12.5, in which we report the detection of C III]${\lambda}{\lambda}$1907,1909 nebular emission. This is the most distant detection of a metal transition and the most distant redshift determination via emission lines. In addition, we report tentative detections of [O II]${\lambda}{\lambda}$3726,3729 and [Ne III]${\lambda}$3869, and possibly O III]${\lambda}{\lambda}$1661,1666. By using the accurate redshift from C III], we can model the Ly${\alpha}$ drop to reliably measure an absorbing column density of hydrogen of $N_{HI} \approx 10^{22}$ cm$^{-2}$ - too high for an IGM origin and implying abundant ISM in GS-z12 or CGM around it. We infer a lower limit for the neutral gas mass of about $10^7$ MSun which, compared with a stellar mass of $\approx4 \times 10^7$ MSun inferred from the continuum fitting, implies a gas fraction higher than about 0.1-0.5. We derive a solar or even super-solar carbon-to-oxygen ratio, tentatively [C/O]>0.15. This is higher than the C/O measured in galaxies discovered by JWST at z=6-9, and higher than the C/O arising from Type-II supernovae enrichment, while AGB stars cannot contribute to carbon enrichment at these early epochs and low metallicities. Such a high C/O in a galaxy observed 350 Myr after the Big Bang may be explained by the yields of extremely metal poor stars, and may even be the heritage of the first generation of supernovae from Population III progenitors., Comment: 13 pages, 8 figures. Submitted to Astronomy & Astrophysics
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- 2023
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119. The galaxies missed by Hubble and ALMA: the contribution of extremely red galaxies to the cosmic census at 3<z<8
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Williams, Christina C., Alberts, Stacey, Ji, Zhiyuan, Hainline, Kevin N., Lyu, Jianwei, Rieke, George, Endsley, Ryan, Suess, Katherine A., Johnson, Benjamin D., Florian, Michael, Shivaei, Irene, Rujopakarn, Wiphu, Baker, William M., Bhatawdekar, Rachana, Boyett, Kristan, Bunker, Andrew J., Carniani, Stefano, Charlot, Stephane, Curtis-Lake, Emma, DeCoursey, Christa, de Graaff, Anna, Egami, Eiichi, Eisenstein, Daniel J., Gibson, Justus L., Hausen, Ryan, Helton, Jakob M., Maiolino, Roberto, Maseda, Michael V., Nelson, Erica J., Perez-Gonzalez, Pablo G., Rieke, Marcia J., Robertson, Brant E., Sun, Fengwu, Tacchella, Sandro, Willmer, Christopher N. A., and Willott, Chris J.
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Astrophysics - Astrophysics of Galaxies - Abstract
Using deep JWST imaging from JADES, JEMS and SMILES, we characterize optically-faint and extremely red galaxies at $z>3$ that were previously missing from galaxy census estimates. The data indicate the existence of abundant, dusty and post-starburst-like galaxies down to $10^8$M$_\odot$, below the sensitivity limit of Spitzer and ALMA. Modeling the NIRCam and HST photometry of these red sources can result in extreme, high values for both stellar mass and star formation rate (SFR); however, including 7 MIRI filters out to 21$\mu$m results in decreased mass (median 0.6 dex for log$_{10}$M$^*$/M$_{\odot}>$10), and SFR (median 10$\times$ for SFR$>$100 M$_{\odot}$/yr). At $z>6$, our sample includes a high fraction of little red dots (LRDs; NIRCam-selected dust-reddened AGN candidates). We significantly measure older stellar populations in the LRDs out to rest-frame 3$\mu$m (the stellar bump) and rule out a dominant contribution from hot dust emission, a signature of AGN contamination to stellar population measurements. This allows us to measure their contribution to the cosmic census at $z>3$, below the typical detection limits of ALMA ($L_{\rm IR}<10^{12}L_\odot$). We find that these sources, which are overwhelmingly missed by HST and ALMA, could effectively double the obscured fraction of the star formation rate density at $4
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- 2023
120. Planetary Radio Interferometry and Doppler Experiment (PRIDE) of the JUICE mission
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Gurvits, Leonid I., Cimo, Giuseppe, Dirkx, Dominic, Pallichadath, Vidhya, Akins, Alexander, Altobelli, Nicolas, Bocanegra-Bahamon, Tatiana M., Cazaux, Stephanie M., Charlot, Patrick, Duev, Dmitry A., Fayolle, Marie S., Fogasy, Judit, Frey, Sandor, Lainey, Valery, Calves, Guifre Molera, Perger, Krisztina, Pogrebenko, Sergey V., Said, N. Masdiana Md, Vallat, Claire, Vermeersen, Bert L. A., Visser, Pieter N. A. M., Wang, Kuo-Nung, and Willner, Konrad
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Physics - Space Physics - Abstract
Planetary Radio Interferometry and Doppler Experiment (PRIDE) is a multi-purpose experimental technique aimed at enhancing the science return of planetary missions. The technique exploits the science payload and spacecraft service systems without requiring a dedicated onboard instrumentation or imposing on the existing instrumentation any special for PRIDE requirements. PRIDE is based on the near-field phase-referencing Very Long Baseline Interferometry (VLBI) and evaluation of the Doppler shift of the radio signal transmitted by spacecraft by observing it with multiple Earth-based radio telescopes. The methodology of PRIDE has been developed initially at the Joint Institute for VLBI ERIC (JIVE) for tracking the ESA's Huygens Probe during its descent in the atmosphere of Titan in 2005. From that point on, the technique has been demonstrated for various planetary and other space science missions. The estimates of lateral position of the target spacecraft are done using the phase-referencing VLBI technique. Together with radial Doppler estimates, these observables can be used for a variety of applications, including improving the knowledge of the spacecraft state vector. The PRIDE measurements can be applied to a broad scope of research fields including studies of atmospheres through the use of radio occultations, the improvement of planetary and satellite ephemerides, as well as gravity field parameters and other geodetic properties of interest, and estimations of interplanetary plasma properties. This paper presents the implementation of PRIDE as a component of the ESA's Jupiter Icy Moons Explorer (JUICE) mission., Comment: Accepted for publication in Space Science Reviews, v. 219 (special issue on the ESA's JUICE mission)
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- 2023
121. JADES: Using NIRCam Photometry to Investigate the Dependence of Stellar Mass Inferences on the IMF in the Early Universe
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Woodrum, Charity, Rieke, Marcia, Ji, Zhiyuan, Baker, William M., Bhatawdekar, Rachana, Bunker, Andrew J., Charlot, Stéphane, Curtis-Lake, Emma, Eisenstein, Daniel J., Hainline, Kevin, Hausen, Ryan, Helton, Jakob M., Hviding, Raphael E., Johnson, Benjamin D., Robertson, Brant, Sun, Fengwu, Tacchella, Sandro, Whitler, Lily, Williams, Christina C., and Willmer, Christopher N. A.
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Astrophysics - Astrophysics of Galaxies - Abstract
The detection of numerous and relatively bright galaxies at redshifts z > 9 has prompted new investigations into the star-forming properties of high-redshift galaxies. Using local forms of the initial mass function (IMF) to estimate stellar masses of these galaxies from their light output leads to galaxy masses that are at the limit allowed for the state of the LambdaCDM Universe at their redshift. We explore how varying the IMF assumed in studies of galaxies in the early universe changes the inferred values for the stellar masses of these galaxies. We infer galaxy properties with the SED fitting code Prospector using varying IMF parameterizations for a sample of 102 galaxies from the JWST Advanced Deep Extragalactic Survey (JADES) spectroscopically confirmed to be at z > 6.7, with additional photometry from the JWST Extragalactic Medium Band Survey (JEMS) for twenty-one galaxies. We demonstrate that models with stellar masses reduced by a factor of three or more do not affect the modeled spectral energy distribution (SED)., Comment: The Significance statement is required for PNAS submission
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- 2023
122. The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
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Eisenstein, Daniel J., Johnson, Benjamin D., Robertson, Brant, Tacchella, Sandro, Hainline, Kevin, Jakobsen, Peter, Maiolino, Roberto, Bonaventura, Nina, Bunker, Andrew J., Cameron, Alex J., Cargile, Phillip A., Curtis-Lake, Emma, Hausen, Ryan, Puskás, Dávid, Rieke, Marcia, Sun, Fengwu, Willmer, Christopher N. A., Willott, Chris, Alberts, Stacey, Arribas, Santiago, Baker, William M., Baum, Stefi, Bhatawdekar, Rachana, Carniani, Stefano, Charlot, Stephane, Chen, Zuyi, Chevallard, Jacopo, Curti, Mirko, DeCoursey, Christa, D'Eugenio, Francesco, de Graaff, Anna, Egami, Eiichi, Helton, Jakob M., Ji, Zhiyuan, Jones, Gareth C., Kumari, Nimisha, Lützgendorf, Nora, Laseter, Isaac, Looser, Tobias J., Lyu, Jianwei, Maseda, Michael V., Nelson, Erica, Parlanti, Eleonora, Rauscher, Bernard J., Rawle, Tim, Rieke, George, Rix, Hans-Walter, Rujopakarn, Wiphu, Sandles, Lester, Saxena, Aayush, Scholtz, Jan, Sharpe, Katherine, Shivaei, Irene, Simmonds, Charlotte, Smit, Renske, Topping, Michael W., Übler, Hannah, Venturi, Giacomo, Williams, Christina C., Witstok, Joris, and Woodrum, Charity
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Astrophysics - Astrophysics of Galaxies - Abstract
We summarize the properties and initial data release of the JADES Origins Field (JOF), which will soon be the deepest imaging field yet observed with the James Webb Space Telescope (JWST). This field falls within the GOODS-S region about 8' south-west of the Hubble Ultra Deep Field (HUDF), where it was formed initially in Cycle 1 as a parallel field of HUDF spectroscopic observations within the JWST Advanced Deep Extragalactic Survey (JADES). This imaging will be greatly extended in Cycle 2 program 3215, which will observe the JOF for 5 days in six medium-band filters, seeking robust candidates for z>15 galaxies. This program will also include ultra-deep parallel NIRSpec spectroscopy (up to 104 hours on-source, summing over the dispersion modes) on the HUDF. Cycle 3 observations from program 4540 will add 20 hours of NIRCam slitless spectroscopy to the JOF. With these three campaigns, the JOF will be observed for 380 open-shutter hours with NIRCam using 15 imaging filters and 2 grism bandpasses. Further, parts of the JOF have deep 43 hr MIRI observations in F770W. Taken together, the JOF will soon be one of the most compelling deep fields available with JWST and a powerful window into the early Universe. This paper presents the second data release from JADES, featuring the imaging and catalogs from the year 1 JOF observations., Comment: Submitted to ApJ Supplement. Images and catalogs are available at https://archive.stsci.edu/hlsp/jades . A FITSmap portal to view the images is at https://jades.idies.jhu.edu
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- 2023
123. Gaia Focused Product Release: Sources from Service Interface Function image analysis -- Half a million new sources in omega Centauri
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Gaia Collaboration, Weingrill, K., Mints, A., Castañeda, J., Kostrzewa-Rutkowska, Z., Davidson, M., De Angeli, F., Hernández, J., Torra, F., Ramos-Lerate, M., Babusiaux, C., Biermann, M., Crowley, C., Evans, D. W., Lindegren, L., Martín-Fleitas, J. M., Palaversa, L., Mieres, D. Ruz, Tisanić, K., Brown, A. G. A., Vallenari, A., Prusti, T., de Bruijne, J. H. J., Arenou, F., Barbier, A., Creevey, O. L., Ducourant, C., Eyer, L., Guerra, R., Hutton, A., Jordi, C., Klioner, S. A., Lammers, U., Luri, X., Mignard, F., Randich, S., Sartoretti, P., Smiljanic, R., Tanga, P., Walton, N. A., Bailer-Jones, C. A. L., Bastian, U., Cropper, M., Drimmel, R., Katz, D., Soubiran, C., van Leeuwen, F., Audard, M., Bakker, J., Blomme, R., Fabricius, C., Fouesneau, M., Frémat, Y., Galluccio, L., Guerrier, A., Masana, E., Messineo, R., Nicolas, C., Nienartowicz, K., Pailler, F., Panuzzo, P., Riclet, F., Roux, W., Seabroke, G. M., Sordo, R., Thévenin, F., Gracia-Abril, G., Portell, J., Teyssier, D., Altmann, M., Benson, K., Berthier, J., Burgess, P. W., Busonero, D., Busso, G., Cánovas, H., Carry, B., Cheek, N., Clementini, G., Damerdji, Y., de Teodoro, P., Delchambre, L., DellÓro, A., Garcia, E. Fraile, Garabato, D., García-Lario, P., Torres, N. Garralda, Gavras, P., Haigron, R., Hambly, N. C., Harrison, D. L., Hatzidimitriou, D., Hodgkin, S. T., Holl, B., Jamal, S., Jordan, S., Krone-Martins, A., Lanzafame, A. C., Löffler, W., Lorca, A., Marchal, O., Marrese, P. M., Moitinho, A., Muinonen, K., Campos, M. Nuñez, Oreshina-Slezak, I., Osborne, P., Pancino, E., Pauwels, T., Recio-Blanco, A., Riello, M., Rimoldini, L., Robin, A. C., Roegiers, T., Sarro, L. M., Schultheis, M., Siopis, C., Smith, M., Sozzetti, A., Utrilla, E., van Leeuwen, M., Abbas, U., Ábrahám, P., Aramburu, A. Abreu, Aerts, C., Altavilla, G., Álvarez, M. A., Alves, J., Anders, F., Anderson, R. I., Antoja, T., Baines, D., Baker, S. G., Balog, Z., Barache, C., Barbato, D., Barros, M., Barstow, M. A., Bartolomé, S., Bashi, D., Bauchet, N., Baudeau, N., Becciani, U., Bedin, L. R., Bellas-Velidis, I., Bellazzini, M., Beordo, W., Berihuete, A., Bernet, M., Bertolotto, C., Bertone, S., Bianchi, L., Binnenfeld, A., Blazere, A., Boch, T., Bombrun, A., Bouquillon, S., Bragaglia, A., Braine, J., Bramante, L., Breedt, E., Bressan, A., Brouillet, N., Brugaletta, E., Bucciarelli, B., Butkevich, A. G., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzo, S., Cantat-Gaudin, T., Carballo, R., Carlucci, T., Carnerero, M. I., Carrasco, J. M., Carretero, J., Carton, S., Casamiquela, L., Castellani, M., Castro-Ginard, A., Cesare, V., Charlot, P., Chemin, L., Chiaramida, V., Chiavassa, A., Chornay, N., Collins, R., Contursi, G., Cooper, W. J., Cornez, T., Crosta, M., Dafonte, C., de Laverny, P., De Luise, F., De March, R., de Souza, R., de Torres, A., del Peloso, E. F., Delbo, M., Delgado, A., Dharmawardena, T. E., Diakite, S., Diener, C., Distefano, E., Dolding, C., Dsilva, K., Durán, J., Enke, H., Esquej, P., Fabre, C., Fabrizio, M., Faigler, S., Fatović, M., Fedorets, G., Fernández-Hernández, J., Fernique, P., Figueras, F., Fournier, Y., Fouron, C., Gai, M., Galinier, M., Garcia-Gutierrez, A., García-Torres, M., Garofalo, A., Gerlach, E., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Gomel, R., Gomez, A., González-Núñez, J., González-Santamaría, I., Gosset, E., Granvik, M., Barrera, V. Gregori, Gutiérrez-Sánchez, R., Haywood, M., Helmer, A., Helmi, A., Henares, K., Hidalgo, S. L., Hilger, T., Hobbs, D., Hottier, C., Huckle, H. E., Jabłońska, M., Jansen, F., Jiménez-Arranz, Ó., Campillo, J. Juaristi, Khanna, S., Kordopatis, G., Kóspál, Á, Kun, M., Lambert, S., Lanza, A. F., Campion, J. -F. Le, Lebreton, Y., Lebzelter, T., Leccia, S., Lecoeur-Taibi, I., Lecoutre, G., Liao, S., Liberato, L., Licata, E., Lindstrøm, H. E. P., Lister, T. A., Livanou, E., Lobel, A., Loup, C., Mahy, L., Mann, R. G., Manteiga, M., Marchant, J. M., Marconi, M., Pina, D. Marín, Marinoni, S., Marshall, D. J., Lozano, J. Martín, Marton, G., Mary, N., Masip, A., Massari, D., Mastrobuono-Battisti, A., Mazeh, T., McMillan, P. J., Meichsner, J., Messina, S., Michalik, D., Millar, N. R., Molina, D., Molinaro, R., Molnár, L., Monari, G., Monguió, M., Montegriffo, P., Montero, A., Mor, R., Mora, A., Morbidelli, R., Morel, T., Morris, D., Mowlavi, N., Munoz, D., Muraveva, T., Murphy, C. P., Musella, I., Nagy, Z., Nieto, S., Noval, L., Ogden, A., Ordenovic, C., Pagani, C., Pagano, I., Palicio, P. A., Pallas-Quintela, L., Panahi, A., Panem, C., Payne-Wardenaar, S., Pegoraro, L., Penttilä, A., Pesciullesi, P., Piersimoni, A. M., Pinamonti, M., Pineau, F. -X., Plachy, E., Plum, G., Poggio, E., Pourbaix, D., Prša, A., Pulone, L., Racero, E., Rainer, M., Raiteri, C. M., Ramos, P., Ratajczak, M., Fiorentin, P. Re, Regibo, S., Reylé, C., Ripepi, V., Riva, A., Rix, H. -W., Rixon, G., Robichon, N., Robin, C., Romero-Gómez, M., Rowell, N., Royer, F., Rybicki, K. A., Sadowski, G., Núñez, A. Sáez, Sellés, A. Sagristà, Sahlmann, J., Gimenez, V. Sanchez, Sanna, N., Santoveña, R., Sarasso, M., Riera, C. Sarrate, Sciacca, E., Segovia, J. C., Ségransan, D., Shahaf, S., Siebert, A., Siltala, L., Slezak, E., Smart, R. L., Snaith, O. N., Solano, E., Solitro, F., Souami, D., Souchay, J., Spina, L., Spitoni, E., Spoto, F., Squillante, L. A., Steele, I. A., Steidelmüller, H., Surdej, J., Szabados, L., Taris, F., Taylor, M. B., Teixeira, R., Tolomei, L., Elipe, G. Torralba, Trabucchi, M., Tsantaki, M., Ulla, A., Unger, N., Vanel, O., Vecchiato, A., Vicente, D., Voutsinas, S., Weiler, M., Wyrzykowski, Ł., Zhao, H., Zorec, J., Zwitter, T., Balaguer-Núñez, L., Leclerc, N., Morgenthaler, S., Robert, G., and Zucker, S.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
Gaia's readout window strategy is challenged by very dense fields in the sky. Therefore, in addition to standard Gaia observations, full Sky Mapper (SM) images were recorded for nine selected regions in the sky. A new software pipeline exploits these Service Interface Function (SIF) images of crowded fields (CFs), making use of the availability of the full two-dimensional (2D) information. This new pipeline produced half a million additional Gaia sources in the region of the omega Centauri ($\omega$ Cen) cluster, which are published with this Focused Product Release. We discuss the dedicated SIF CF data reduction pipeline, validate its data products, and introduce their Gaia archive table. Our aim is to improve the completeness of the {\it Gaia} source inventory in a very dense region in the sky, $\omega$ Cen. An adapted version of {\it Gaia}'s Source Detection and Image Parameter Determination software located sources in the 2D SIF CF images. We validated the results by comparing them to the public {\it Gaia} DR3 catalogue and external Hubble Space Telescope data. With this Focused Product Release, 526\,587 new sources have been added to the {\it Gaia} catalogue in $\omega$ Cen. Apart from positions and brightnesses, the additional catalogue contains parallaxes and proper motions, but no meaningful colour information. While SIF CF source parameters generally have a lower precision than nominal {\it Gaia} sources, in the cluster centre they increase the depth of the combined catalogue by three magnitudes and improve the source density by a factor of ten. This first SIF CF data publication already adds great value to the {\it Gaia} catalogue. It demonstrates what to expect for the fourth {\it Gaia} catalogue, which will contain additional sources for all nine SIF CF regions.
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- 2023
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124. Gaia Focused Product Release: A catalogue of sources around quasars to search for strongly lensed quasars
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Gaia Collaboration, Krone-Martins, A., Ducourant, C., Galluccio, L., Delchambre, L., Oreshina-Slezak, I., Teixeira, R., Braine, J., Campion, J. -F. Le, Mignard, F., Roux, W., Blazere, A., Pegoraro, L., Brown, A. G. A., Vallenari, A., Prusti, T., de Bruijne, J. H. J., Arenou, F., Babusiaux, C., Barbier, A., Biermann, M., Creevey, O. L., Evans, D. W., Eyer, L., Guerra, R., Hutton, A., Jordi, C., Klioner, S. A., Lammers, U., Lindegren, L., Luri, X., Randich, S., Sartoretti, P., Smiljanic, R., Tanga, P., Walton, N. A., Bailer-Jones, C. A. L., Bastian, U., Cropper, M., Drimmel, R., Katz, D., Soubiran, C., van Leeuwen, F., Audard, M., Bakker, J., Blomme, R., Castaneda, J., De Angeli, F., Fabricius, C., Fouesneau, M., Fremat, Y., Guerrier, A., Masana, E., Messineo, R., Nicolas, C., Nienartowicz, K., Pailler, F., Panuzzo, P., Riclet, F., Seabroke, G. M., Sordo, R., Thevenin, F., Gracia-Abril, G., Portell, J., Teyssier, D., Altmann, M., Benson, K., Berthier, J., Burgess, P. W., Busonero, D., Busso, G., Canovas, H., Carry, B., Cheek, N., Clementini, G., Damerdji, Y., Davidson, M., de Teodoro, P., Dell'Oro, A., Garcia, E. Fraile, Garabato, D., Garcia-Lario, P., Torres, N. Garralda, Gavras, P., Haigron, R., Hambly, N. C., Harrison, D. L., Hatzidimitriou, D., Hernandez, J., Hodgkin, S. T., Holl, B., Jamal, S., Jordan, S., Lanzafame, A. C., Loffler, W., Lorca, A., Marchal, O., Marrese, P. M., Moitinho, A., Muinonen, K., Campos, M. Nunez, Osborne, P., Pancino, E., Pauwels, T., Recio-Blanco, A., Riello, M., Rimoldini, L., Robin, A. C., Roegiers, T., Sarro, L. M., Schultheis, M., Siopis, C., Smith, M., Sozzetti, A., Utrilla, E., van Leeuwen, M., Weingrill, K., Abbas, U., Abraham, P., Aramburu, A. Abreu, Aerts, C., Altavilla, G., Alvarez, M. A., Alves, J., Anderson, R. I., Antoja, T., Baines, D., Baker, S. G., Balog, Z., Barache, C., Barbato, D., Barros, M., Barstow, M. A., Bartolome, S., Bashi, D., Bauchet, N., Baudeau, N., Becciani, U., Bedin, L. R., Bellas-Velidis, I., Bellazzini, M., Beordo, W., Berihuete, A., Bernet, M., Bertolotto, C., Bertone, S., Bianchi, L., Binnenfeld, A., Boch, T., Bombrun, A., Bouquillon, S., Bragaglia, A., Bramante, L., Breedt, E., Bressan, A., Brouillet, N., Brugaletta, E., Bucciarelli, B., Butkevich, A. G., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzo, S., Carballo, R., Carlucci, T., Carnerero, M. I., Carrasco, J. M., Carretero, J., Carton, S., Casamiquela, L., Castellani, M., Castro-Ginard, A., Cesare, V., Charlot, P., Chemin, L., Chiaramida, V., Chiavassa, A., Chornay, N., Collins, R., Contursi, G., Cooper, W. J., Cornez, T., Crosta, M., Crowley, C., Dafonte, C., de Laverny, P., De Luise, F., De March, R., de Souza, R., de Torres, A., del Peloso, E. F., Delbo, M., Delgado, A., Dharmawardena, T. E., Diakite, S., Diener, C., Distefano, E., Dolding, C., Dsilva, K., Duran, J., Enke, H., Esquej, P., Fabre, C., Fabrizio, M., Faigler, S., Fatovic, M., Fedorets, G., Fernandez-Hernandez, J., Fernique, P., Figueras, F., Fournier, Y., Fouron, C., Gai, M., Galinier, M., Garcia-Gutierrez, A., Garcia-Torres, M., Garofalo, A., Gerlach, E., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Gomel, R., Gomez, A., Gonzalez-Nunez, J., Gonzalez-Santamaria, I., Gosset, E., Granvik, M., Barrera, V. Gregori, Gutierrez-Sanchez, R., Haywood, M., Helmer, A., Helmi, A., Henares, K., Hidalgo, S. L., Hilger, T., Hobbs, D., Hottier, C., Huckle, H. E., Jablonska, M., Jansen, F., Jimenez-Arranz, O., Campillo, J. Juaristi, Khanna, S., Kordopatis, G., Kospal, A., Kostrzewa-Rutkowska, Z., Kun, M., Lambert, S., Lanza, A. F., Lebreton, Y., Lebzelter, T., Leccia, S., Lecoeur-Taibi, I., Lecoutre, G., Liao, S., Liberato, L., Licata, E., Lindstrom, H. E. P., Lister, T. A., Livanou, E., Lobel, A., Loup, C., Mahy, L., Mann, R. G., Manteiga, M., Marchant, J. M., Marconi, M., Pina, D. Marin, Marinoni, S., Marshall, D. J., Lozano, J. Martin, Martin-Fleitas, J. M., Marton, G., Mary, N., Masip, A., Massari, D., Mastrobuono-Battisti, A., Mazeh, T., McMillan, P. J., Meichsner, J., Messina, S., Michalik, D., Millar, N. R., Mints, A., Molina, D., Molinaro, R., Molnar, L., Monari, G., Monguio, M., Montegriffo, P., Montero, A., Mor, R., Mora, A., Morbidelli, R., Morel, T., Morris, D., Mowlavi, N., Munoz, D., Muraveva, T., Murphy, C. P., Musella, I., Nagy, Z., Nieto, S., Noval, L., Ogden, A., Ordenovic, C., Pagani, C., Pagano, I., Palaversa, L., Palicio, P. A., Pallas-Quintela, L., Panahi, A., Panem, C., Payne-Wardenaar, S., Penttila, A., Pesciullesi, P., Piersimoni, A. M., Pinamonti, M., Pineau, F. -X., Plachy, E., Plum, G., Poggio, E., Pourbaix, D., Prsa, A., Pulone, L., Racero, E., Rainer, M., Raiteri, C. M., Ramos, P., Ramos-Lerate, M., Ratajczak, M., Fiorentin, P. Re, Regibo, S., Reyle, C., Ripepi, V., Riva, A., Rix, H. -W., Rixon, G., Robichon, N., Robin, C., Romero-Gomez, M., Rowell, N., Royer, F., Mieres, D. Ruz, Rybicki, K. A., Sadowski, G., Nunez, A. Saez, Selles, A. Sagrista, Sahlmann, J., Gimenez, V. Sanchez, Sanna, N., Santovena, R., Sarasso, M., Riera, C. Sarrate, Sciacca, E., Segovia, J. C., Segransan, D., Shahaf, S., Siebert, A., Siltala, L., Slezak, E., Smart, R. L., Snaith, O. N., Solano, E., Solitro, F., Souami, D., Souchay, J., Spina, L., Spitoni, E., Spoto, F., Squillante, L. A., Steele, I. A., Steidelmuller, H., Surdej, J., Szabados, L., Taris, F., Taylor, M. B., Tisanic, K., Tolomei, L., Torra, F., Elipe, G. Torralba, Trabucchi, M., Tsantaki, M., Ulla, A., Unger, N., Vanel, O., Vecchiato, A., Vicente, D., Voutsinas, S., Weiler, M., Wyrzykowski, L., Zhao, H., Zorec, J., Zwitter, T., Balaguer-Nunez, L., Leclerc, N., Morgenthaler, S., Robert, G., and Zucker, S.
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Context. Strongly lensed quasars are fundamental sources for cosmology. The Gaia space mission covers the entire sky with the unprecedented resolution of $0.18$" in the optical, making it an ideal instrument to search for gravitational lenses down to the limiting magnitude of 21. Nevertheless, the previous Gaia Data Releases are known to be incomplete for small angular separations such as those expected for most lenses. Aims. We present the Data Processing and Analysis Consortium GravLens pipeline, which was built to analyse all Gaia detections around quasars and to cluster them into sources, thus producing a catalogue of secondary sources around each quasar. We analysed the resulting catalogue to produce scores that indicate source configurations that are compatible with strongly lensed quasars. Methods. GravLens uses the DBSCAN unsupervised clustering algorithm to detect sources around quasars. The resulting catalogue of multiplets is then analysed with several methods to identify potential gravitational lenses. We developed and applied an outlier scoring method, a comparison between the average BP and RP spectra of the components, and we also used an extremely randomised tree algorithm. These methods produce scores to identify the most probable configurations and to establish a list of lens candidates. Results. We analysed the environment of 3 760 032 quasars. A total of 4 760 920 sources, including the quasars, were found within 6" of the quasar positions. This list is given in the Gaia archive. In 87\% of cases, the quasar remains a single source, and in 501 385 cases neighbouring sources were detected. We propose a list of 381 lensed candidates, of which we identified 49 as the most promising. Beyond these candidates, the associate tables in this Focused Product Release allow the entire community to explore the unique Gaia data for strong lensing studies further., Comment: 35 pages, 60 figures, accepted for publication by Astronomy and Astrophysics
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- 2023
- Full Text
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125. FRESCO: An extended, massive, rapidly rotating galaxy at z=5.3
- Author
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Nelson, Erica J., Brammer, Gabriel, Gimenez-Arteaga, Clara, Oesch, Pascal A., Ubler, Hannah, de Graaff, Anna, Matharu, Jasleen, Naidu, Rohan P., Shapley, Alice E., Whitaker, Katherine E., Wisnioski, Emily, Schreiber, Natascha M. Forster, Smit, Renske, van Dokkum, Pieter, Chisholm, John, Endsley, Ryan, Hartley, Abigail I., Gibson, Justus, Giovinazzo, Emma, Illingworth, Garth, Labbe, Ivo, Maseda, Michael V., Matthee, Jorryt, Paz, Alba Covelo, Price, Sedona H., Reddy, Naveen A., Shivaei, Irene, Weibel, Andrea, Wuyts, Stijn, Xiao, Mengyuan, Alberts, Stacey, Baker, William M., Bunker, Andrew J., Cameron, Alex J., Charlot, Stephane, Eisenstein, Daniel J., Ji, Zhiyuan, Johnson, Benjamin D., Jones, Gareth C., Maiolino, Roberto, Robertson, Brant, Sandles, Lester, Suess, Katherine A., Tacchella, Sandro, Williams, Christina C., and Witstok, Joris
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Astrophysics - Astrophysics of Galaxies - Abstract
With the remarkable sensitivity and resolution of JWST in the infrared, measuring rest-optical kinematics of galaxies at $z>5$ has become possible for the first time. This study pilots a new method for measuring galaxy dynamics for highly multiplexed, unbiased samples by combining FRESCO NIRCam grism spectroscopy and JADES medium-band imaging. Here we present one of the first JWST kinematic measurements for a galaxy at $z>5$. We find a significant velocity gradient, which, if interpreted as rotation yields $V_{rot} = 240\pm50$km/s and we hence refer to this galaxy as Twister-z5. With a rest-frame optical effective radius of $r_e=2.25$kpc, the high rotation velocity in this galaxy is not due to a compact size as may be expected in the early universe but rather a high total mass, ${\rm log(M}_{dyn}/{\rm M}_\odot)=11.0\pm0.2$. This is a factor of roughly 4x higher than the stellar mass within the effective radius. We also observe that the radial H$\alpha$ equivalent width profile and the specific star formation rate map from resolved stellar population modeling is centrally depressed by a factor of $\sim1.5$ from the center to $r_e$. Combined with the morphology of the line-emitting gas in comparison to the continuum, this centrally suppressed star formation is consistent with a star-forming disk surrounding a bulge growing inside-out. While large, rapidly rotating disks are common to z~2, the existence of one after only 1Gyr of cosmic time, shown for the first time in ionized gas, adds to the growing evidence that some galaxies matured earlier than expected in the history of the universe., Comment: Fig. 3 shows the main result
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- 2023
126. Gaia Focused Product Release: Radial velocity time series of long-period variables
- Author
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Gaia Collaboration, Trabucchi, M., Mowlavi, N., Lebzelter, T., Lecoeur-Taibi, I., Audard, M., Eyer, L., García-Lario, P., Gavras, P., Holl, B., de Fombelle, G. Jevardat, Nienartowicz, K., Rimoldini, L., Sartoretti, P., Blomme, R., Frémat, Y., Marchal, O., Damerdji, Y., Brown, A. G. A., Guerrier, A., Panuzzo, P., Katz, D., Seabroke, G. M., Benson, K., Haigron, R., Smith, M., Lobel, A., Vallenari, A., Prusti, T., de Bruijne, J. H. J., Arenou, F., Babusiaux, C., Barbier, A., Biermann, M., Creevey, O. L., Ducourant, C., Evans, D. W., Guerra, R., Hutton, A., Jordi, C., Klioner, S. A., Lammers, U., Lindegren, L., Luri, X., Mignard, F., Randich, S., Smiljanic, R., Tanga, P., Walton, N. A., Bailer-Jones, C. A. L., Bastian, U., Cropper, M., Drimmel, R., Lattanzi, M. G., Soubiran, C., van Leeuwen, F., Bakker, J., Castañeda, J., De Angeli, F., Fabricius, C., Fouesneau, M., Galluccio, L., Masana, E., Messineo, R., Nicolas, C., Pailler, F., Riclet, F., Roux, W., Sordo, R., Thévenin, F., Gracia-Abril, G., Portell, J., Teyssier, D., Altmann, M., Berthier, J., Burgess, P. W., Busonero, D., Busso, G., Cánovas, H., Carry, B., Cheek, N., Clementini, G., Davidson, M., de Teodoro, P., Delchambre, L., Dell'Oro, A., Garcia, E. Fraile, Garabato, D., Torres, N. Garralda, Hambly, N. C., Harrison, D. L., Hatzidimitriou, D., Hernández, J., Hodgkin, S. T., Jamal, S., Jordan, S., Krone-Martins, A., Lanzafame, A. C., Löffler, W., Lorca, A., Marrese, P. M., Moitinho, A., Muinonen, K., Campos, M. Nuñez, Oreshina-Slezak, I., Osborne, P., Pancino, E., Pauwels, T., Recio-Blanco, A., Riello, M., Robin, A. C., Roegiers, T., Sarro, L. M., Schultheis, M., Siopis, C., Sozzetti, A., Utrilla, E., van Leeuwen, M., Weingrill, K., Abbas, U., Ábrahám, P., Aramburu, A. Abreu, Aerts, C., Altavilla, G., Álvarez, M. A., Alves, J., Anders, F., Anderson, R. I., Antoja, T., Baines, D., Baker, S. G., Balog, Z., Barache, C., Barbato, D., Barros, M., Barstow, M. A., Bartolomé, S., Bashi, D., Bauchet, N., Baudeau, N., Becciani, U., Bedin, L. R., Bellas-Velidis, I., Bellazzini, M., Beordo, W., Berihuete, A., Bernet, M., Bertolotto, C., Bertone, S., Bianchi, L., Binnenfeld, A., Blazere, A., Boch, T., Bombrun, A., Bouquillon, S., Bragaglia, A., Braine, J., Bramante, L., Breedt, E., Bressan, A., Brouillet, N., Brugaletta, E., Bucciarelli, B., Butkevich, A. G., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzo, S., Carballo, R., Carlucci, T., Carnerero, M. I., Carrasco, J. M., Carretero, J., Carton, S., Casamiquela, L., Castellani, M., Castro-Ginard, A., Cesare, V., Charlot, P., Chemin, L., Chiaramida, V., Chiavassa, A., Chornay, N., Collins, R., Contursi, G., Cooper, W. J., Cornez, T., Crosta, M., Crowley, C., Dafonte, C., David, M., de Laverny, P., De Luise, F., De March, R., De Ridder, J., de Souza, R., de Torres, A., del Peloso, E. F., Delbo, M., Delgado, A., Dharmawardena, T. E., Diakite, S., Diener, C., Distefano, E., Dolding, C., Dsilva, K., Durán, J., Enke, H., Esquej, P., Fabre, C., Fabrizio, M., Faigler, S., Fatović, M., Fedorets, G., Fernández-Hernández, J., Fernique, P., Figueras, F., Fournier, Y., Fouron, C., Gai, M., Galinier, M., Garcia-Gutierrez, A., García-Torres, M., Garofalo, A., Gerlach, E., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Gomel, R., Gomez, A., González-Núñez, J., González-Santamaría, I., Gosset, E., Granvik, M., Barrera, V. Gregori, Gutiérrez-Sánchez, R., Haywood, M., Helmer, A., Helmi, A., Henares, K., Hidalgo, S. L., Hilger, T., Hobbs, D., Hottier, C., Huckle, H. E., Jabłońska, M., Jansen, F., Jiménez-Arranz, Ó., Campillo, J. Juaristi, Khanna, S., Kordopatis, G., Kóspál, Á, Kostrzewa-Rutkowska, Z., Kun, M., Lambert, S., Lanza, A. F., Campion, J. -F. Le, Lebreton, Y., Leccia, S., Lecoutre, G., Liao, S., Liberato, L., Licata, E., Lindstrøm, H. E. P., Lister, T. A., Livanou, E., Loup, C., Mahy, L., Mann, R. G., Manteiga, M., Marchant, J. M., Marconi, M., Pina, D. Marín, Marinoni, S., Marshall, D. J., Lozano, J. Martín, Martín-Fleitas, J. M., Marton, G., Mary, N., Masip, A., Massari, D., Mastrobuono-Battisti, A., Mazeh, T., McMillan, P. J., Meichsner, J., Messina, S., Michalik, D., Millar, N. R., Mints, A., Molina, D., Molinaro, R., Molnár, L., Monari, G., Monguió, M., Montegriffo, P., Montero, A., Mor, R., Mora, A., Morbidelli, R., Morel, T., Morris, D., Munoz, D., Muraveva, T., Murphy, C. P., Musella, I., Nagy, Z., Nieto, S., Noval, L., Ogden, A., Ordenovic, C., Pagani, C., Pagano, I., Palaversa, L., Palicio, P. A., Pallas-Quintela, L., Panahi, A., Panem, C., Payne-Wardenaar, S., Pegoraro, L., Penttilä, A., Pesciullesi, P., Piersimoni, A. M., Pinamonti, M., Pineau, F. -X., Plachy, E., Plum, G., Poggio, E., Pourbaix, D., Prša, A., Pulone, L., Racero, E., Rainer, M., Raiteri, C. M., Ramos, P., Ramos-Lerate, M., Ratajczak, M., Fiorentin, P. Re, Regibo, S., Reylé, C., Ripepi, V., Riva, A., Rix, H. -W., Rixon, G., Robichon, N., Robin, C., Romero-Gómez, M., Rowell, N., Royer, F., Mieres, D. Ruz, Rybicki, K. A., Sadowski, G., Núñez, A. Sáez, Sellés, A. Sagristà, Sahlmann, J., Gimenez, V. Sanchez, Sanna, N., Santoveña, R., Sarasso, M., Riera, C. Sarrate, Sciacca, E., Segovia, J. C., Ségransan, D., Shahaf, S., Siebert, A., Siltala, L., Slezak, E., Smart, R. L., Snaith, O. N., Solano, E., Solitro, F., Souami, D., Souchay, J., Spina, L., Spitoni, E., Spoto, F., Squillante, L. A., Steele, I. A., Steidelmüller, H., Surdej, J., Szabados, L., Taris, F., Taylor, M. B., Teixeira, R., Tisanić, K., Tolomei, L., Torra, F., Elipe, G. Torralba, Tsantaki, M., Ulla, A., Unger, N., Vanel, O., Vecchiato, A., Vicente, D., Voutsinas, S., Weiler, M., Wyrzykowski, Ł., Zhao, H., Zorec, J., Zwitter, T., Balaguer-Núñez, L., Leclerc, N., Morgenthaler, S., Robert, G., and Zucker, S.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
The third Gaia Data Release (DR3) provided photometric time series of more than 2 million long-period variable (LPV) candidates. Anticipating the publication of full radial-velocity (RV) in DR4, this Focused Product Release (FPR) provides RV time series for a selection of LPVs with high-quality observations. We describe the production and content of the Gaia catalog of LPV RV time series, and the methods used to compute variability parameters published in the Gaia FPR. Starting from the DR3 LPVs catalog, we applied filters to construct a sample of sources with high-quality RV measurements. We modeled their RV and photometric time series to derive their periods and amplitudes, and further refined the sample by requiring compatibility between the RV period and at least one of the $G$, $G_{\rm BP}$, or $G_{\rm RP}$ photometric periods. The catalog includes RV time series and variability parameters for 9\,614 sources in the magnitude range $6\lesssim G/{\rm mag}\lesssim 14$, including a flagged top-quality subsample of 6\,093 stars whose RV periods are fully compatible with the values derived from the $G$, $G_{\rm BP}$, and $G_{\rm RP}$ photometric time series. The RV time series contain a mean of 24 measurements per source taken unevenly over a duration of about three years. We identify the great most sources (88%) as genuine LPVs, with about half of them showing a pulsation period and the other half displaying a long secondary period. The remaining 12% consists of candidate ellipsoidal binaries. Quality checks against RVs available in the literature show excellent agreement. We provide illustrative examples and cautionary remarks. The publication of RV time series for almost 10\,000 LPVs constitutes, by far, the largest such database available to date in the literature. The availability of simultaneous photometric measurements gives a unique added value to the Gaia catalog (abridged), Comment: 36 pages, 38 figures
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- 2023
127. HST FUV Spectroscopy of Super Star Cluster A in the Green Pea Analog Mrk 71: Revealing the Presence of Very Massive Stars
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Smith, Linda J., Oey, M. S., Hernandez, Svea, Ryon, Jenna, Leitherer, Claus, Charlot, Stephane, Bruzual, Gustavo, Calzetti, Daniela, Chu, You-Hua, Hayes, Matthew J., James, Bethan L., Jaskot, Anne. E., and Oestlin, Goeran
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Astrophysics - Astrophysics of Galaxies - Abstract
Mrk 71 is a low metallicity (Z = 0.16 Z_sun) starburst region in the local dwarf galaxy NGC 2366, hosting two super star clusters (SSCs A and B), and is recognized as a Green Pea (GP) analog with SSC A responsible for the GP properties. We present STIS and FOS far-ultraviolet (FUV) spectra of the embedded SSC Mrk 71-A obtained with the Hubble Space Telescope (HST). The STIS FUV spectrum shows the characteristic features of very massive stars (VMS, masses > 100 M_sun) and we derive an age of 1+/-1 Myr by comparison with the Charlot & Bruzual suite of spectral population synthesis models with upper mass limits of 300 and 600 M_sun. We compare the STIS spectrum with all known SSC spectra exhibiting VMS signatures: NGC 5253-5, R136a, NGC 3125-A1 and the z = 2.37 Sunburst cluster. We find that the cluster mass-loss rates and wind velocities, as characterized by the C IV P Cygni profiles and the He II emission line strengths, are very similar over Z = 0.16 to 0.4 Z_sun. This agrees with predictions that the optically thick winds of VMS will be enhanced near the Eddington limit and show little metallicity dependence. We find very strong damped Lyman-alpha absorption with log N(H I) = 22.2 cm-2 associated with Mrk 71-A. We discuss the natal environment of this young SSC in terms of radiatively-driven winds, catastrophic cooling and recent models where the cluster is surrounded by highly pressurized clouds with large neutral columns., Comment: 15 pages accepted for publication in the Astrophysical Journal
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- 2023
128. GA-NIFS: A high number of dual AGN at z~3
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Perna, Michele, Arribas, Santiago, Lamperti, Isabella, Circosta, Chiara, Bertola, Elena, Pérez-González, Pablo G., D'Eugenio, Francesco, Übler, Hannah, Cresci, Giovanni, Volonteri, Marta, Mannucci, Filippo, Maiolino, Roberto, Del Pino, Bruno Rodríguez, Bunker, Andrew J., Charlot, Stéphane, Willott, Chris J., Carniani, Stefano, Böker, Torsten, Curti, Mirko, Jones, Gareth, Kumari, Nimisha, Marshall, Madeline A., Saxena, Aayush, Scholtz, Jan, Venturi, Giacomo, and Witstok, Joris
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Astrophysics - Astrophysics of Galaxies - Abstract
Merger events can trigger gas accretion onto supermassive black holes (SMBHs) located at the centre of galaxies, and form close pairs of AGN. The fraction of AGN in pairs offers critical insights into the dynamics of galaxy interactions, SMBH growth, and their co-evolution with host galaxies. However, the identification of dual AGN is difficult, as it requires high-quality spatial and spectral data; hence, only very few pairs have been found in the distant Universe so far. This study aims to provide a first observational estimate of the fraction of dual AGN at 2
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- 2023
129. Low-mass bursty galaxies in JADES efficiently produce ionising photons and could represent the main drivers of reionisation
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Simmonds, C., Tacchella, S., Hainline, K., Johnson, B. D., McClymont, W., Robertson, B., Saxena, A., Sun, F., Witten, C., Baker, W. M., Bhatawdekar, R., Boyett, K., Bunker, A. J., Charlot, S., Curtis-Lake, E., Egami, E., Eisenstein, D. J., Hausen, R., Maiolino, R., Maseda, M. V., Scholtz, J., Williams, C. C., Willot, C., and Witstok, J.
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Astrophysics - Astrophysics of Galaxies - Abstract
We study galaxies in JADES Deep to study the evolution of the ionising photon production efficiency, $\xi_{\rm{ion}}$, observed to increase with redshift. We estimate $\xi_{\rm{ion}}$ for a sample of 677 galaxies at $z \sim 4 - 9$ using NIRCam photometry. Specifically, combinations of the medium and wide bands F335M-F356W and F410M-F444W to constrain emission lines that trace $\xi_{\rm{ion}}$: H$\alpha$ and [OIII]. Additionally, we use the spectral energy distribution fitting code \texttt{Prospector} to fit all available photometry and infer galaxy properties. The flux measurements obtained via photometry are consistent with FRESCO and NIRSpec-derived fluxes. Moreover, the emission-line-inferred measurements are in tight agreement with the \texttt{Prospector} estimates. We also confirm the observed $\xi_{\rm{ion}}$ trend with redshift and M$_{\rm{UV}}$, and find: $\log \xi_{\rm{ion}} (z,\text{M}_{\rm{UV}}) = (0.05 \pm 0.02)z + (0.11 \pm 0.02) \text{M}_{\rm{UV}} + (27.33 \pm 0.37)$. We use \texttt{Prospector} to investigate correlations of $\xi_{\rm{ion}}$ with other galaxy properties. We see a clear correlation between $\xi_{\rm{ion}}$ and burstiness in the star formation history of galaxies, given by the ratio of recent to older star formation, where burstiness is more prevalent at lower stellar masses. We also convolve our $\xi_{\rm{ion}}$ relations with luminosity functions from the literature, and constant escape fractions of 10 and 20\%, to place constraints on the cosmic ionising photon budget. By combining our results, we find that if our sample is representative of the faint low-mass galaxy population, galaxies with bursty star formation are efficient enough in producing ionising photons and could be responsible for the reionisation of the Universe., Comment: Submitted to MNRAS. 19 pages, 14 figures
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- 2023
130. A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): JWST Discovers an Overdensity around a Metal Absorption-selected Galaxy at $z\sim5.5$
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Wu, Yunjing, Wang, Feige, Cai, Zheng, Fan, Xiaohui, Finlator, Kristian, Yang, Jinyi, Hennawi, Joseph F., Sun, Fengwu, Champagne, Jaclyn B., Lin, Xiaojing, Li, Zihao, Chen, Zuyi, Bañados, Eduardo, Becker, George D., Bosman, Sarah E. I., Bruzual, Gstavo, Charlot, Stephane, Chen, Hsiao-Wen, Chevallard, Jacopo, Eilers, Anna-Christina, Farina, Emanuele Paolo, Jin, Xiangyu, Jun, Hyunsung D., Kakiichi, Koki, Li, Mingyu, Liu, Weizhe, Pudoka, Maria A., Tee, Wei Leong, Xie, Zhang-Liang, and Zou, Siwei
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The launch of ${\it JWST}$ opens a new window for studying the connection between metal-line absorbers and galaxies at the end of the Epoch of Reionization (EoR). Previous studies have detected absorber-galaxy pairs in limited quantities through ground-based observations. To enhance our understanding of the relationship between absorbers and their host galaxies at $z>5$, we utilized the NIRCam Wide Field Slitless Spectroscopy (WFSS) to search for absorber-associated galaxies by detecting their rest-frame optical emission lines (e.g., [OIII] + H$\beta$). We report the discovery of a MgII-associated galaxy at $z=5.428$ using data from the ${\it JWST}$ ASPIRE program. The MgII absorber is detected on the spectrum of quasar J0305--3150 with a rest-frame equivalent width of 0.74$\mathring{A}$. The associated galaxy has an [OIII] luminosity of $10^{42.5}\ {\rm erg\ s^{-1}}$ with an impact parameter of 24.9 proper kiloparsecs (pkpc). The joint ${\it HST}$-${\it JWST}$ spectral energy distribution (SED) implies a stellar mass and star-formation rate of ${\rm M_* \approx 10^{8.8}}$ ${\rm M_{\odot}}$, ${\rm SFR}\approx 10\ {\rm M_{\odot}\ yr^{-1}}$. Its [OIII] equivalent width and stellar mass are typical of [OIII] emitters at this redshift. Furthermore, connecting the outflow starting time to the SED-derived stellar age, the outflow velocity of this galaxy is $\sim300\ {\rm km\ s^{-1}}$, consistent with theoretical expectations. We identified six additional [OIII] emitters with impact parameters of up to $\sim300$ pkpc at similar redshifts ($|dv|<1000\ {\rm km\ s^{-1}}$). The observed number is consistent with that in cosmological simulations. This pilot study suggests that systematically investigating the absorber-galaxy connection within the ASPIRE program will provide insights into the metal-enrichment history in the early universe., Comment: Accepted for publication in ApJL. Main text 8 pages, 4 figures. For more information of the JWST ASPIRE program please check https://aspire-quasar.github.io/index.html
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- 2023
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131. GA-NIFS: co-evolution within a highly star-forming galaxy group at z=3.7 witnessed by JWST/NIRSpec IFS
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Del Pino, B. Rodríguez, Perna, M., Arribas, S., D'Eugenio, F., Lamperti, I., Pérez-González, P. G., Übler, H., Bunker, A., Carniani, S., Charlot, S., Maiolino, R., Willott, C. J., Böker, T., Chevallard, J., Cresci, G., Curti, M., Jones, G. C., Parlanti, E., Scholtz, J., and Venturi, G.
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Astrophysics - Astrophysics of Galaxies - Abstract
We present NIRSpec IFS observations of a galaxy group around the massive GS_4891 galaxy at z=3.7 in GOODS-South that includes two other two systems, GS_4891_n to the north and GS_28356 to the east. These observations, obtained as part of the GTO GA-NIFS program, allow for the first time to study the spatially resolved properties of the interstellar medium (ISM) and ionized gas kinematics of a galaxy at this redshift. Leveraging the wide wavelength range spanned with the high-dispersion grating (with resolving power R=2700) observations, covering from [OII]$\lambda$$\lambda$3726,29 to [SII]$\lambda$$\lambda$6716,31, we explore the spatial distribution of star-formation rate, nebular attenuation and gas metallicity, together with the mechanisms responsible for the excitation of the ionized gas. GS_4891 presents a clear gradient of gas metallicity (as traced by 12 + log(O/H)) by more than 0.2dex from the south-east (where a star-forming clump is identified) to the north-west. The gas metallicity in the less-massive northern system, GS_4891_n, is also higher by 0.2 dex than at the center of GS_4891, suggesting that inflows of lower-metallicity gas might be favoured in higher-mass systems. The kinematic analysis shows that GS_4891 presents velocity gradients in the ionized gas consistent with rotation. The region between GS_4891 and GS_4891_n does not present high gas turbulence which, together with the difference in gas metallicities, suggests that these two systems might be in a pre-merger stage. Finally, GS_4891 hosts an ionized outflow that extends out to r_out=1.2 kpc from the nucleus and reaches maximum velocities v_out of approximately 400 km/s. Despite entraining an outflowing mass rate of M_out$\sim$2Msun/yr, the low associated mass-loading factor, $\eta$=0.05, implies that the outflow does not have a significant impact on the star-formation activity of the galaxy., Comment: Submitted to Astronomy & Astrophysics on September 25th, 2023
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- 2023
132. Neuromuscular and Metabolic Responses during Repeated Bouts of Loaded Downhill Walking
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Chalchat, Emeric, Siracusa, Julien, Peñailillo, Luis, Malgoyre, Alexandra, Bourrilhon, Cyprien, Charlot, Keyne, Martin, Vincent, and Garcia-Vicencio, Sebastian
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Quantitative Biology - Tissues and Organs - Abstract
The aim of this study was to compare vastus lateralis (VL) and rectus femoris (RF) muscles for their nervous and mechanical adaptations during two bouts of downhill walking (DW) with load carriage performed two weeks apart. Moreover, we investigated cardio-metabolic and perceived exertion responses during both DW bouts. Methods Seventeen participants performed two 45-min sessions of loaded DW (30% of body mass; slope: -25 %; speed: 4.5 km$\times$h -1 ) separated by two weeks. Rating of perceived exertion (RPE), cost of walking (C w ), heart rate (HR), and EMG activity of thigh muscles were assessed during the DW. Muscle shear elastic modulus ($\mu$) of RF and VL were assessed before each exercise bout. Maximal voluntary contraction (MVC) torque was assessed before (PRE), immediately after (POST), 24 and 48 h after the two exercise bouts. Results MVC torque decreased from POST (-23.7 $\pm$ 9.2%) to 48 h (-19.2 $\pm$ 11.9%) after the first exercise (Ex1), whereas it was significantly reduced only at POST (-14.6 $\pm$ 11.0%) after the second exercise (Ex2) (p < 0.001). RPE (Ex1: 12.3 $\pm$ 1.9; Ex2: 10.8 $\pm$ 2.0), HR (Ex1: 156 $\pm$ 23 bpm; Ex2: 145 $\pm$ 25 bpm), C w (Ex1: 4.5 $\pm$ 0.9 J$\times$m -1 $\times$kg -1 ; Ex2: 4.1 $\pm$ 0.7 J$\times$m -1 $\times$kg -1 ) and RF EMG activity (Ex1: 0.071 $\pm$ 0.028 mV; Ex2: 0.041 $\pm$ 0.014 mV) were significantly decreased during Ex2 compared to Ex1 (p < 0.01). RF $\mu$ was significantly greater in Ex2 (0.44 $\pm$ 0.18) compared to Ex1 (0.56 $\pm$ 0.27; p < 0.001). Conclusions The RF muscle displayed specific mechanical and nervous adaptations to repeated DW bouts as compared to VL. Moreover, the muscle adaptations conferred by the first bout of DW could have induced greater exercise efficiency, inducing lesser perceived exertion and cardio-metabolic demand when the same exercise was repeated two weeks later., Comment: Medicine and Science in Sports and Exercise, 2023
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- 2023
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133. Metal enrichment and evolution in four z > 6.5 quasar sightlines observed with JWST/NIRSpec
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Christensen, L., Jakobsen, P., Willott, C., Arribas, S., Bunker, A., Charlot, S., Maiolino, R., Marshall, M., Perna, M., and Übler, H.
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Astrophysics - Astrophysics of Galaxies - Abstract
We present JWST/NIRSpec R~2700 spectra of four high-redshift quasars: VDES J0020-3653 (z = 6.860), DELS J0411-0907 (z = 6.825), UHS J0439+1634 (z = 6.519) and ULAS J1342+0928 (z = 7.535). The exquisite data quality, signal-to-noise ratio of 50-200, and large $0.86\!~\mu{\rm m}\le \lambda \le 5.5\!~\mu{\rm m}$ spectral coverage allows us to identify between 13 and 17 intervening and proximate metal absorption line systems in each quasar spectrum, with a total number of 61 absorption-line systems detected at 2.42
6 and find: i) A continued increase of the low-ionization OI, CII, and SiII incidence, ii) Decreasing high-ionization CIV and SiIV incidence with a transition from predominantly high- to low-ionization at $z\approx6.0$, and iii) a constant MgII incidence across all redshifts. The observations support a change in the ionization state of the intergalactic medium in the EoR rather than a change in metallicity. The abundance ratio of [Si/O] in five z>6 absorption systems show enrichment signatures produced by low-mass Pop III pair instability supernovae, and possibly Pop III hypernovae. In the Gunn-Peterson troughs we detect transmission spikes where Ly$\alpha$ photons can escape. From 22 absorption systems at z>5.7, only a single low-ionization system out of 13 lies within 2000 km/s from a spike, while four high-ionization systems out of nine lie within ~2000 km/s from a spike. This confirms that galaxies responsible for the heavy elements that are transported into the circumgalactic medium lie in predominantly in high-density, neutral environments, while lower density environments are ionized without being polluted by metals at $z\approx$ 6-7. [abridged], Comment: 48 pages including 28 pages of appendices. Accepted for publication in A&A - Published
- 2023
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134. GA-NIFS: Early-stage feedback in a heavily obscured AGN at $z=4.76$
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Parlanti, Eleonora, Carniani, Stefano, Übler, Hannah, Venturi, Giacomo, Circosta, Chiara, D'Eugenio, Francesco, Arribas, Santiago, Bunker, Andrew J., Charlot, Stéphane, Lützgendorf, Nora, Maiolino, Roberto, Perna, Michele, Del Pino, Bruno Rodríguez, Willott, Chris J., Böker, Torsten, Cameron, Alex J., Chevallard, Jacopo, Cresci, Giovanni, Jones, Gareth C., Kumari, Nimisha, Lamperti, Isabella, and Scholtz, Jan
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Dust-obscured galaxies are thought to represent an early evolutionary phase of massive galaxies in which the active galactic nucleus (AGN) is still deeply buried in significant amounts of dusty material and its emission is strongly suppressed. The unprecedented sensitivity of the James Webb Space Telescope enables us for the first time to detect the rest-frame optical emission of heavily obscured AGN and unveil the properties of the hidden accreting super-massive black holes (BHs). In this work, we present the JWST/NIRSpec IFS data of ALESS073.1, a massive, dusty, star-forming galaxy at $z = 4.76$ hosting an AGN at its center. The detection of a very broad $H_\alpha$ emission associated with the Broad Line Region (BLR) confirms the presence of a BH ($\log(M_{BH}/M_\odot)>8.7$) accreting at less than 15\% of its Eddington limit and classifies the target as a Type 1 AGN. The rest-frame optical emission lines also reveal a fast ionized gas outflow marginally resolved in the galaxy center. The high sensitivity of NIRSpec allows us to perform the kinematic analysis of the narrow H$\alpha$ component which indicates that the warm ionized gas velocity field is consistent with disk rotation. We also find that, in the innermost nuclear regions ($< 1.5$ kpc), the intrinsic velocity dispersion of the disk reaches $\sim 150$ km/s, $\sim 2-3$ times higher than the velocity dispersion inferred from the [CII] 158$\mu$m line tracing mostly cold gas. Since, at large radii, the velocity dispersion of the warm and cold gas are comparable, we conclude that the outflows are injecting turbulence in the warm ionized gas in the central region, but they are not sufficiently powerful to disrupt the dense gas and quench star formation. These findings support the scenario that dust-obscured galaxies represent the evolutionary stage preceding the unobscured quasar when all gas and dust are removed from the host., Comment: 16 pages, 12 figures, accepted in A&A
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- 2023
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135. JADES: Resolving the Stellar Component and Filamentary Overdense Environment of HST-Dark Submillimeter Galaxy HDF850.1 at $z=5.18$
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Sun, Fengwu, Helton, Jakob M., Egami, Eiichi, Hainline, Kevin N., Rieke, George H., Willmer, Christopher N. A., Eisenstein, Daniel J., Johnson, Benjamin D., Rieke, Marcia J., Robertson, Brant, Tacchella, Sandro, Alberts, Stacey, Baker, William M., Bhatawdekar, Rachana, Boyett, Kristan, Bunker, Andrew J., Charlot, Stephane, Chen, Zuyi, Chevallard, Jacopo, Curtis-Lake, Emma, Danhaive, A. Lola, DeCoursey, Christa, Ji, Zhiyuan, Lyu, Jianwei, Maiolino, Roberto, Rujopakarn, Wiphu, Sandles, Lester, Shivaei, Irene, Ubler, Hannah, Willott, Chris, and Witstok, Joris
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Astrophysics - Astrophysics of Galaxies - Abstract
HDF850.1 is the brightest submillimeter galaxy (SMG) in the Hubble Deep Field. It is known as a heavily dust-obscured star-forming galaxy embedded in an overdense environment at $z = 5.18$. With nine-band NIRCam images at 0.8-5.0 $\mu$m obtained through the JWST Advanced Deep Extragalactic Survey (JADES), we detect and resolve the rest-frame UV-optical counterpart of HDF850.1, which splits into two components because of heavy dust obscuration in the center. The southern component leaks UV and H$\alpha$ photons, bringing the galaxy $\sim$100 times above the empirical relation between infrared excess and UV continuum slope (IRX-$\beta_\mathrm{UV}$). The northern component is higher in dust attenuation and thus fainter in UV and H$\alpha$ surface brightness. We construct a spatially resolved dust attenuation map from the NIRCam images, well matched with the dust continuum emission obtained through millimeter interferometry. The whole system hosts a stellar mass of $10^{10.8\pm0.1}\,\mathrm{M}_\odot$ and star-formation rate of $10^{2.8\pm0.2}\,\mathrm{M}_\odot\,\mathrm{yr}^{-1}$, placing the galaxy at the massive end of the star-forming main sequence at this epoch. We further confirm that HDF850.1 resides in a complex overdense environment at $z=5.17-5.30$, which hosts another luminous SMG at $z=5.30$ (GN10). The filamentary structures of the overdensity are characterized by 109 H$\alpha$-emitting galaxies confirmed through NIRCam slitless spectroscopy at 3.9-5 $\mu$m, of which only eight were known before the JWST observations. Given the existence of a similar galaxy overdensity in the GOODS-S field, our results suggest that $50\pm20$% of the cosmic star formation at $z=5.1-5.5$ occur in protocluster environments., Comment: 44 pages, 16 figures, 2 tables. Accepted for publication in ApJ
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- 2023
136. CLASSY. VIII. Exploring the Source of Ionization with UV Interstellar Medium Diagnostics in Local High-z Analogs* *Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
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Mingozzi, Matilde, James, Bethan L, Berg, Danielle A, Arellano-Córdova, Karla Z, Plat, Adele, Scarlata, Claudia, Aloisi, Alessandra, Amorín, Ricardo O, Brinchmann, Jarle, Charlot, Stéphane, Chisholm, John, Feltre, Anna, Gazagnes, Simon, Hayes, Matthew, Heckman, Timothy, Hernandez, Svea, Kewley, Lisa J, Kumari, Nimisha, Leitherer, Claus, Martin, Crystal L, Maseda, Michael, Nanayakkara, Themiya, Ravindranath, Swara, Rigby, Jane R, Senchyna, Peter, Skillman, Evan D, Sugahara, Yuma, Wilkins, Stephen M, Wofford, Aida, and Xu, Xinfeng
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Space Sciences ,Physical Sciences ,Astronomical and Space Sciences ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry (incl. Structural) ,Astronomy & Astrophysics ,Astronomical sciences ,Particle and high energy physics ,Space sciences - Abstract
Abstract: In the current JWST era, rest-frame UV spectra play a crucial role in enhancing our understanding of the interstellar medium (ISM) and stellar properties of the first galaxies in the epoch of reionization (z > 6). Here, we compare well-known and reliable optical diagrams sensitive to the main ionization source (i.e., star formation, SF; active galactic nuclei, AGN; and shocks) to UV counterparts proposed in the literature—the so-called “UV–BPT diagrams”—using the HST COS Legacy Archive Spectroscopic SurveY (CLASSY), which is the largest high-quality, high-resolution, and broad-wavelength range atlas of far-UV spectra for 45 local star-forming galaxies. In particular, we explore where CLASSY UV line ratios are located in the different UV diagnostic plots, taking into account state-of-the-art photoionization and shock models, and, for the first time, the measured ISM and stellar properties (e.g., gas-phase metallicity, ionization parameter, carbon abundance, and stellar age). We find that the combination of C iii] λ λ1907,9 He ii λ1640 and O iii] λ1666 can be a powerful tool to separate between SF, shocks, and AGN at subsolar metallicities. We also confirm that alternative diagrams without O iii] λ1666 still allow us to define an SF-locus, with some caveats. Diagrams including C iv λ λ1548,51 should be taken with caution given the complexity of this doublet profile. Finally, we present a discussion detailing the ISM conditions required to detect UV emission lines, visible only in low gas-phase metallicity (12 + log(O/H) ≲ 8.3) and high ionization parameter (log(U) ≳ −2.5) environments. Overall, CLASSY and our UV toolkit will be crucial in interpreting the spectra of the earliest galaxies that JWST is currently revealing.
- Published
- 2024
137. GA-NIFS: JWST/NIRSpec IFU observations of HFLS3 reveal a dense galaxy group at z~6.3
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Jones, G. C., Ubler, H., Perna, M., Arribas, S., Bunker, A. J., Carniani, S., Charlot, S., Maiolino, R., Del Pino, B. Rodriguez, Willott, C., Bowler, R. A. A., Boker, T., Cameron, A. J., Chevallard, J., Cresci, G., Curti, M., D'Eugenio, F., Kumari, N., Saxena, A., Scholtz, J., Venturi, G., and Witstok, J.
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
Massive, starbursting galaxies in the early Universe represent some of the most extreme objects in the study of galaxy evolution. One such source is HFLS3 (z~6.34), which was originally identified as an extreme starburst galaxy with mild gravitational magnification ($\mu$~2.2). Here, we present new observations of HFLS3 with the JWST/NIRSpec IFU in both low (PRISM/CLEAR; R~100) and high spectral resolution (G395H/290LP; R~2700), with high spatial resolution (~0.1") and sensitivity. Thanks to the combination of the NIRSpec data and a new lensing model with accurate spectroscopic redshifts, we find that the 3"x3" field is crowded, with a lensed arc (C, $z=6.3425\pm0.0002$), two galaxies to the south (S1 and S2, $z=6.3592\pm0.0001$), two galaxies to the west (W1, $z=6.3550\pm0.0001$; W2, $z=6.3628\pm0.0001$), and two low-redshift interlopers (G1, $z=3.4806\pm0.0001$; G2, $z=2.00\pm0.01$). We present spectral fits and morpho-kinematic maps for each bright emission line from the R2700 data for all sources except G2. From a line ratio analysis, the galaxies in component C are likely powered by star formation, while we cannot rule out or confirm the presence of AGN in the other high-redshift sources. We perform gravitational lens modelling, finding evidence for a two-source composition of the lensed central object and a comparable magnification factor ($\mu$=2.1-2.4) to previous work. The projected distances and velocity offsets of each galaxy suggest that they will merge within the next ~1Gyr. Finally, we examine the dust extinction-corrected SFR(Ha) of each z>6 source, finding that the total star formation ($510\pm140$Msol/yr, magnification-corrected) is distributed across the six z~6.34-6.36 objects over a region of diameter ~11kpc. Altogether, this suggests that HFLS3 is not a single starburst galaxy, but instead is a merging system of star-forming galaxies in the Epoch of Reionisation., Comment: 27 pages, 17 figures, accepted for publication in A&A
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- 2023
138. Ionised gas kinematics and dynamical masses of $z\gtrsim6$ galaxies from JADES/NIRSpec high-resolution spectroscopy
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de Graaff, Anna, Rix, Hans-Walter, Carniani, Stefano, Suess, Katherine A., Charlot, Stéphane, Curtis-Lake, Emma, Arribas, Santiago, Baker, William M., Boyett, Kristan, Bunker, Andrew J., Cameron, Alex J., Chevallard, Jacopo, Curti, Mirko, Eisenstein, Daniel J., Franx, Marijn, Hainline, Kevin, Hausen, Ryan, Ji, Zhiyuan, Johnson, Benjamin D., Jones, Gareth C., Maiolino, Roberto, Maseda, Michael V., Nelson, Erica, Parlanti, Eleonora, Rawle, Tim, Robertson, Brant, Tacchella, Sandro, Übler, Hannah, Williams, Christina C., Willmer, Christopher N. A., and Willott, Chris
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Astrophysics - Astrophysics of Galaxies - Abstract
We explore the kinematic gas properties of six $5.5
1$ thus far. The cold gas masses implied by the observed star formation rates are $\sim 10\times$ larger than the stellar masses. We find that their ionised gas is spatially resolved by JWST, with evidence for broadened lines and spatial velocity gradients. Using a simple thin-disc model, we fit these data with a novel forward modelling software that accounts for the complex geometry, point spread function, and pixellation of the NIRSpec instrument. We find the sample to include both rotation- and dispersion-dominated structures, as we detect velocity gradients of $v(r_{\rm e})\approx100-150\,{\rm km\,s^{-1}}$, and find velocity dispersions of $\sigma_0\approx 30-70\,{\rm km\,s^{-1}}$ that are comparable to those at cosmic noon. The dynamical masses implied by these models ($M_{\rm dyn}\sim10^{9-10}\,{\rm M_\odot}$) are larger than the stellar masses by up to a factor 40, and larger than the total baryonic mass (gas + stars) by a factor of $\sim 3$. Qualitatively, this result is robust even if the observed velocity gradients reflect ongoing mergers rather than rotating discs. Unless the observed emission line kinematics is dominated by outflows, this implies that the centres of these galaxies are dark-matter dominated or that star formation is $3\times$ less efficient, leading to higher inferred gas masses., Comment: Accepted for publication in A&A. Software for JWST/NIRSpec MSA modelling (slit losses, 1D LSFs and 2D model fitting) publicly available at https://github.com/annadeg/jwst-msafit - Published
- 2023
139. A fast-rotator post-starburst galaxy quenched by supermassive black-hole feedback at z=3
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D'Eugenio, Francesco, Perez-Gonzalez, Pablo, Maiolino, Roberto, Scholtz, Jan, Perna, Michele, Circosta, Chiara, Uebler, Hannah, Arribas, Santiago, Boeker, Torsten, Bunker, Andrew, Carniani, Stefano, Charlot, Stephane, Chevallard, Jacopo, Cresci, Giovanni, Curtis-Lake, Emma, Jones, Gareth, Kumari, Nimisha, Lamperti, Isabella, Looser, Tobias, Parlanti, Eleonora, Rix, Hans-Walter, Robertson, Brant, Del Pino, Bruno Rodriguez, Tacchella, Sandro, Venturi, Giacomo, and Willott, Chris
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Astrophysics - Astrophysics of Galaxies - Abstract
There is compelling evidence that the most massive galaxies in the Universe stopped forming stars due to the time-integrated feedback from their central super-massive black holes (SMBHs). However, the exact quenching mechanism is not yet understood, because local massive galaxies were quenched billions of years ago. We present JWST/NIRSpec integral-field spectroscopy observations of GS-10578, a massive, quiescent galaxy at redshift z=3.064. From the spectrum we infer that the galaxy has a stellar mass of $M_*=1.6\pm0.2 \times 10^{11}$ MSun and a dynamical mass $M_{\rm dyn}=2.0\pm0.5 \times 10^{11}$ MSun. Half of its stellar mass formed at z=3.7-4.6, and the system is now quiescent, with the current star-formation rate SFR<9 MSun/yr. We detect ionised- and neutral-gas outflows traced by [OIII] emission and NaI absorption. Outflow velocities reach $v_{\rm out}\approx$1,000 km/s, comparable to the galaxy escape velocity and too high to be explained by star formation alone. GS-10578 hosts an Active Galactic Nucleus (AGN), evidence that these outflows are due to SMBH feedback. The outflow rates are 0.14-2.9 and 30-300 MSun/yr for the ionised and neutral phases, respectively. The neutral outflow rate is ten times higher than the SFR, hence this is direct evidence for ejective SMBH feedback, with mass-loading capable of interrupting star formation by rapidly removing its fuel. Stellar kinematics show ordered rotation, with spin parameter $\lambda_{Re}=0.62\pm0.07$, meaning GS-10578 is rotation supported. This study shows direct evidence for ejective AGN feedback in a massive, recently quenched galaxy, thus clarifying how SMBHs quench their hosts. Quenching can occur without destroying the stellar disc., Comment: 40 pages, 9 figures, submitted to Nat. Ast., comments welcome!
- Published
- 2023
140. A high black hole to host mass ratio in a lensed AGN in the early Universe
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Furtak, Lukas J., Labbé, Ivo, Zitrin, Adi, Greene, Jenny E., Dayal, Pratika, Chemerynska, Iryna, Kokorev, Vasily, Miller, Tim B., Goulding, Andy D., de Graaff, Anna, Bezanson, Rachel, Brammer, Gabriel B., Cutler, Sam E., Leja, Joel, Pan, Richard, Price, Sedona H., Wang, Bingjie, Weaver, John R., Whitaker, Katherine E., Atek, Hakim, Bogdán, Ákos, Charlot, Stéphane, Curtis-Lake, Emma, van Dokkum, Pieter, Endsley, Ryan, Fudamoto, Yoshinobu, Fujimoto, Seiji, Glazebrook, Karl, Juneau, Stéphanie, Marchesini, Danilo, Maseda, Michael V., Nelson, Erica, Oesch, Pascal A., Plat, Adèle, Setton, David J., Stark, Daniel P., and Williams, Christina C.
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
Early JWST observations have uncovered a new population of red sources that might represent a previously overlooked phase of supermassive black hole growth (Kocevski et al. 2023; Matthee et al. 2023, Labb\'e et al. 2023). One of the most intriguing examples is an extremely red, point-like object that was found to be triply-imaged by the strong lensing (SL) cluster Abell 2744 (Furtak et al. 2023). Here we present deep JWST/NIRSpec observations of this object, Abell2744-QSO1. The spectroscopy confirms that the three images are of the same object, and that it is a highly reddened ($A_V\simeq3$) broad emission-line Active Galactic Nucleus (AGN) at a redshift of $z_{\mathrm{spec}}=7.0451\pm0.0005$. From the width of H$\beta$ ($\mathrm{FWHM}=2800\pm250\,\frac{\mathrm{km}}{\mathrm{s}}$) we derive a black hole mass of $M_{\mathrm{BH}}=4_{-1}^{+2}\times10^7\,\mathrm{M}_{\odot}$. We infer a very high ratio of black hole to galaxy mass of at least 3%, an order of magnitude more than is seen in local galaxies (Bennert et al. 2011), and possibly as high as 100%. The lack of strong metal lines in the spectrum together with the high bolometric luminosity ($L_{\mathrm{bol}}=(1.1\pm0.3)\times10^{45}\,\frac{\mathrm{erg}}{\mathrm{s}}$) indicate that we are seeing the black hole in a phase of rapid growth, accreting at 30% of the Eddington limit. The rapid growth and high black hole to galaxy mass ratio of A2744-QSO1 suggest that it may represent the missing link between black hole seeds (Volonteri et al. 2021) and the first luminous quasars (Fan et al. 2022)., Comment: Published in Nature. Updated to the accepted version
- Published
- 2023
141. JADES. The diverse population of infant Black Holes at 4<z<11: merging, tiny, poor, but mighty
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Maiolino, Roberto, Scholtz, Jan, Curtis-Lake, Emma, Carniani, Stefano, Baker, William, de Graaff, Anna, Tacchella, Sandro, Übler, Hannah, D'Eugenio, Francesco, Witstok, Joris, Curti, Mirko, Arribas, Santiago, Bunker, Andrew J., Charlot, Stéphane, Chevallard, Jacopo, Eisenstein, Daniel J., Egami, Eiichi, Ji, Zhiyuan, Jones, Gareth C., Lyu, Jianwei, Rawle, Tim, Robertson, Brant, Rujopakarn, Wiphu, Perna, Michele, Sun, Fengwu, Venturi, Giacomo, Williams, Christina C., and Willott, Chris
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
We present 12 new AGN at 4
10^44 erg/s, among galaxies in the redshift range 4 10%., Comment: Accepted for publication in A&A. 26 pages, 13 figures, 4 tables. Replaced with the accepted version (minor changes) - Published
- 2023
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142. Minor merger growth in action: JWST detects faint blue companions around massive quiescent galaxies at 0.5 < z < 3
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Suess, Katherine A., Williams, Christina C., Robertson, Brant, Ji, Zhiyuan, Johnson, Benjamin D., Nelson, Erica, Alberts, Stacey, Hainline, Kevin, DEugenio, Francesco, Ubler, Hannah, Rieke, Marcia, Rieke, George, Bunker, Andrew J., Carniani, Stefano, Charlot, Stephane, Eisenstein, Daniel J., Maiolino, Roberto, Stark, Daniel P., Tacchella, Sandro, and Willott, Chris
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Astrophysics - Astrophysics of Galaxies - Abstract
Minor mergers are thought to drive the structural evolution of massive quiescent galaxies; however, existing HST imaging is primarily sensitive to stellar mass ratios >1:10. Here, we report the discovery of a large population of low-mass companions within 35 kpc of known logM*/Msun > 10.5 quiescent galaxies at 0.5 < z < 3. While massive companions like those identified by HST are rare, JWST imaging from JADES reveals that the average massive quiescent galaxy hosts ~5 nearby companions with stellar mass ratios <1:10. Despite a median stellar mass ratio of just 1:900, these tiny companions are so numerous that they represent at least 30\% of the total mass being added to quiescent galaxies via minor mergers. While relatively massive companions have colors similar to their hosts, companions with mass ratios <1:10 typically have bluer colors and lower mass-to-light ratios than their host galaxies at similar radii. The accretion of these tiny companions is likely to drive evolution in the color gradients and stellar population properties of the host galaxies. Our results suggest that the well-established ``minor merger growth" model for quiescent galaxies extends down to very low mass ratios of <1:100, and demonstrates the power of JWST to constrain both the spatially-resolved properties of massive galaxies and the properties of low-mass companions beyond the local universe., Comment: 10 pages, 5 figures, submitted to ApJL. Comments welcome
- Published
- 2023
143. JADES: deep spectroscopy of a low-mass galaxy at redshift 2.3 quenched by environment
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Sandles, Lester, D'Eugenio, Francesco, Helton, Jakob M., Maiolino, Roberto, Hainline, Kevin, Baker, William M., Williams, Christina C., Alberts, Stacey, Bunker, Andrew J., Carniani, Stefano, Charlot, Stephane, Chevallard, Jacopo, Curti, Mirko, Curtis-Lake, Emma, Eisenstein, Daniel J., Ji, Zhiyuan, Johnson, Benjamin D., Looser, Tobias J., Rawle, Tim, Robertson, Brant, Del Pino, Bruno Rodríguez, Tacchella, Sandro, Übler, Hannah, Willmer, Christopher N. A., and Willott, Chris
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Astrophysics - Astrophysics of Galaxies - Abstract
We report the discovery of a quiescent galaxy at $z=2.34$ with a stellar mass of only $M_\star = 9.5^{+1.8}_{-1.2} \times 10^{8} \mathrm{M}_\odot$, based on deep JWST/NIRSpec spectroscopy. This is the least massive quiescent galaxy found so far at high redshift. We use a Bayesian approach to model the spectrum and photometry, and find the target to have been quiescent for 0.6 Gyr with a mass-weighted average stellar age of 0.8-1.7 Gyr (dominated by systematics). The galaxy displays an inverse colour gradient with radius, consistent with environment-driven quenching. Based on a combination of spectroscopic and robust (medium- and broad-band) photometric redshifts, we identify a galaxy overdensity near the location of the target (5-$\sigma$ above the background level at this redshift). We stress that had we been specifically targetting galaxies within overdensities, the main target would not have been selected on photometry alone; therefore, environment studies based on photometric redshifts are biased against low-mass quiescent galaxies. The overdensity contains three spectroscopically confirmed, massive, old galaxies ($M_\star = 8-17 \times 10^{10} \mathrm{M}_\odot$). The presence of these evolved systems points to accelerated galaxy evolution in overdensities at redshifts z > 2, in agreement with previous works. In projection, our target lies only 35 pkpc away from the most massive galaxy in this overdensity (spectroscopic redshift z = 2.349) which is located close to overdensity's centre. This suggests the low-mass galaxy was quenched by environment, making it possibly the earliest evidence for environment-driven quenching to date., Comment: Submitted to A&A
- Published
- 2023
144. The UV Continuum Slopes of Early Star-Forming Galaxies in JADES
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Topping, Michael W., Stark, Daniel P., Endsley, Ryan, Whitler, Lily, Hainline, Kevin, Johnson, Benjamin D., Robertson, Brant, Tacchella, Sandro, Chen, Zuyi, Alberts, Stacey, Baker, William M., Bunker, Andrew J., Carniani, Stefano, Charlot, Stephane, Chevallard, Jacopo, Curtis-Lake, Emma, DeCoursey, Christa, Egami, Eiichi, Eisenstein, Daniel J., Ji, Zhiyuan, Maiolino, Roberto, Williams, Christina C., Willmer, Christopher N. A., Willott, Chris, and Witstok, Joris
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
The power-law slope of the rest-UV continuum ($f_{\lambda}\propto\lambda^{\beta}$) is a key metric of early star forming galaxies, providing one of our only windows into the stellar populations and physical conditions of $z>10$ galaxies. Expanding upon previous studies with limited sample sizes, we leverage deep imaging from JADES to investigate the UV slopes of 179 $z>9$ galaxies with apparent magnitudes of $m_{\rm F200W}=26-31$, which display a median UV slope of $\beta=-2.4$. We compare to a statistical sample of $z=5-9$ galaxies, finding a shift toward bluer rest-UV colors at all $\rm~M_{UV}$. The most UV-luminous $z>9$ galaxies are significantly bluer than their lower-redshift counterparts, representing a dearth of moderately-red galaxies in the first $500~$Myr. At yet earlier times, the $z>11$ galaxy population exhibits very blue UV slopes, implying very low attenuation from dust. We identify a robust sample of 44 galaxies with $\beta<-2.8$, which have SEDs requiring models of density-bounded HII regions and median ionizing photon escape fractions of $0.51$ to reproduce. Their rest-optical colors imply that this sample has weaker emission lines (median $m_{\rm F356W}-m_{\rm F444W}=0.19$ mag) than typical galaxies (median $m_{\rm F356W}-m_{\rm F444W}=0.39$ mag), consistent with the inferred escape fractions. This sample has relatively low stellar masses (median $\log(M/M_{\odot})=7.5$), and specific star-formation rates (median$=79\rm/Gyr$) nearly twice that of our full sample (median$=44\rm/Gyr$), suggesting they are more common among systems experiencing a recent upturn in star formation. We demonstrate that the shutoff of star formation provides an alternative solution for modelling of extremely blue UV colors, making distinct predictions for the rest-optical emission of these galaxies. Future spectroscopy will be required to distinguish between these physical pictures., Comment: 17 pages, 13 figures; submitted to MNRAS
- Published
- 2023
145. CLASSY VIII: Exploring the Source of Ionization with UV ISM diagnostics in local High-$z$ Analogs
- Author
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Mingozzi, Matilde, James, Bethan L., Berg, Danielle A., Arellano-Córdova, Karla Z., Plat, Adele, Scarlata, Claudia, Aloisi, Alessandra, Amorín, Ricardo O., Brinchmann, Jarle, Charlot, Stéphane, Chisholm, John, Feltre, Anna, Gazagnes, Simon, Hayes, Matthew, Heckman, Timothy, Hernandez, Svea, Kewley, Lisa J., Kumari, Nimisha, Leitherer, Claus, Martin, Crystal L., Maseda, Michael, Nanayakkara, Themiya, Ravindranath, Swara, Rigby, Jane R., Senchyna, Peter, Skillman, Evan D., Sugahara, Yuma, Wilkins, Stephen M., Wofford, Aida, and Xu, Xinfeng
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
In the current JWST era, rest-frame UV spectra play a crucial role in enhancing our understanding of the interstellar medium (ISM) and stellar properties of the first galaxies in the epoch of reionization (EoR, $z>6$). Here, we compare well-known and reliable optical diagrams sensitive to the main ionization source (i.e., star formation, SF; active galactic nuclei, AGN; shocks) to UV counterparts proposed in the literature - the so-called ``UV-BPT diagrams'' - using the HST COS Legacy Archive Spectroscopic SurveY (CLASSY), the largest high-quality, high-resolution and broad-wavelength range atlas of far-UV spectra for 45 local star-forming galaxies. In particular, we explore where CLASSY UV line ratios are located in the different UV diagnostic plots, taking into account state-of-the-art photoionization and shock models and, for the first time, the measured ISM and stellar properties (e.g., gas-phase metallicity, ionization parameter, carbon abundance, stellar age). We find that the combination of C III] $\lambda\lambda$1907,9 He II $\lambda1640$ and O III] $\lambda$1666 can be a powerful tool to separate between SF, shocks and AGN at sub-solar metallicities. We also confirm that alternative diagrams without O III] $\lambda$1666 still allow us to define a SF-locus with some caveats. Diagrams including C IV $\lambda\lambda$1548,51 should be taken with caution given the complexity of this doublet profile. Finally, we present a discussion detailing the ISM conditions required to detect UV emission lines, visible only in low gas-phase metallicity (12+log(O/H) $\lesssim8.3$) and high ionization parameter (log($U$) $\gtrsim-2.5$) environments. Overall, CLASSY and our UV toolkit will be crucial in interpreting the spectra of the earliest galaxies that JWST is currently revealing., Comment: 36 pages, 15 figures, accepted for publication in ApJ
- Published
- 2023
146. JADES: The incidence rate and properties of galactic outflows in low-mass galaxies across 3 < z < 9
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Carniani, Stefano, Venturi, Giacomo, Parlanti, Eleonora, de Graaff, Anna, Maiolino, Roberto, Arribas, Santiago, Bonaventura, Nina, Boyett, Kristan, Bunker, Andrew J., Cameron, Alex J., Charlot, Stephane, Chevallard, Jacopo, Curti, Mirko, Curtis-Lake, Emma, Eisenstein, Daniel J., Giardino, Giovanna, Hausen, Ryan, Kumari, Nimisha, Maseda, Michael V., Nelson, Erica, Perna, Michele, Rix, Hans-Walter, Robertson, Brant, Del Pino, Bruno Rodríguez, Sandles, Lester, Scholtz, Jan, Simmonds, Charlotte, Smit, Renske, Tacchella, Sandro, Übler, Hannah, Williams, Christina C., Willott, Chris, and Witstok, Joris
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
We investigate the incidence and properties of ionized gas outflows in a sample of 52 galaxies with stellar mass between $10^7$ M$_{\odot}$ and $10^9$ M$_{\odot}$ observed with ultra-deep JWST/NIRSpec MSA spectroscopy as part of the JWST Advanced Deep Extragalactic Survey (JADES). The high-spectral resolution (R2700) NIRSpec observations allowed us to identify for the first time the signature of outflows in the rest-frame optical nebular lines in low-mass galaxies at $z>3$. The incidence fraction of ionized outflows, traced by broad components, is about 25-40$\%$ depending on the intensity of the emission lines. The low incidence fraction might be due to both the sensitivity limit and the fact that outflows are not isotropic but have a limited opening angle which results in a detection only when this is directed toward our line of sight. Evidence for outflows increases slightly with stellar mass and star-formation rate. The median velocity and mass loading factor (i.e., the ratio between mass outflow rate and star formation rate) of the outflowing ionized gas are 350 km s$^{-1}$ and $\eta=2.0^{+1.6}_{-1.5}$, respectively. These are 1.5 and 100 times higher, respectively than the typical values observed in local dwarf galaxies. These outflows are able to escape the gravitational potential of the galaxy and enrich the circum-galactic medium and, potentially, the inter-galactic medium. Our results indicate that outflows can significantly impact the star formation activity in low-mass galaxies within the first 2 Gyr of the Universe., Comment: 16 pages, 3 tables
- Published
- 2023
- Full Text
- View/download PDF
147. GN-z11: The environment of an AGN at $z=$10.603
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Scholtz, Jan, Witten, Callum, Laporte, Nicolas, Ubler, Hannah, Perna, Michele, Maiolino, Roberto, Arribas, Santiago, Baker, William, Bennett, Jake, D'Eugenio, Francesco, Tacchella, Sandro, Witstok, Joris, Bunker, Andrew, Carniani, Stefano, Charlot, Stephane, Cresci, Giovanni, Curtis-Lake, Emma, Eisenstein, Daniel, Kumari, Nimisha, Robertson, Brant, Del Pino, Bruno Rodriguez, Simmonds, Charlotte, Smit, Renske, Venturi, Giacomo, Williams, Christina, and Willmer, Christopher
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
Recent observations with the \textit{James Webb} Space Telescope (JWST) have further refined the spectroscopic redshift of GN-z11, one of the most distant galaxies identified with the \textit{Hubble} Space Telescope (HST) at $z=10.603$. The presence of extremely dense gas ($>10^{10}$ cm$^{-3}$), the detection of high-ionisation lines and of CII*1335 emission, as well as the presence of an ionisation cone, indicate that GN-z11 also hosts an Active Galactic Nucleus (AGN). Further photometric and spectroscopic follow-up demonstrates that it lies in a large-scale, overdense structure with possible signatures of Population III (PopIII) stars in its halo. Surprisingly, Ly$\alpha$ has also been detected despite the expected largely neutral inter-galactic medium at such a redshift. We exploit recent JWST/NIRSpec IFU observations to demonstrate that the Ly$\alpha$ emission in GN-z11 is part of an extended halo with a minimum size of 0.8--3.2 kpc, depending on the definition used to derive the halo size. The surface brightness of the Ly$\alpha$ halo around GN-z11 appears consistent with Ly$\alpha$ halos observed around $z\sim6$ quasars. At the wavelength of Ly$\alpha$ at $z\sim$10.6, we identify three other emission line candidates within the IFU Field-of-View with no UV rest-frame counterpart visible in deep images from the JWST/NIRCam. If confirmed, this could be the first evidence that the local region of GN-z11 represents a candidate protocluster core, forming just 400 Myr after the Big Bang. We give a first estimate of the dark matter halo mass of this structure ($M_h$=2.96$^{+0.44}_{-0.39} \times$10$^{10}$ M$_{\odot}$), consistent with a Coma-like cluster progenitor., Comment: Submitted to A&A. 8 pages, 5 figures
- Published
- 2023
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148. The Star-forming and Ionizing Properties of Dwarf z~6-9 Galaxies in JADES: Insights on Bursty Star Formation and Ionized Bubble Growth
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Endsley, Ryan, Stark, Daniel P., Whitler, Lily, Topping, Michael W., Johnson, Benjamin D., Robertson, Brant, Tacchella, Sandro, Alberts, Stacey, Baker, William M., Bhatawdekar, Rachana, Boyett, Kristan, Bunker, Andrew J., Cameron, Alex J., Carniani, Stefano, Charlot, Stéphane, Chen, Zuyi, Chevallard, Jacopo, Curtis-Lake, Emma, Danhaive, A. Lola, Egami, Eiichi, Eisenstein, Daniel J., Hainline, Kevin, Helton, Jakob M., Ji, Zhiyuan, Looser, Tobias J., Maiolino, Roberto, Nelson, Erica, Puskás, Dávid, Rieke, George, Rieke, Marcia, Rix, Hans-Walter, Sandles, Lester, Saxena, Aayush, Simmonds, Charlotte, Smit, Renske, Sun, Fengwu, Williams, Christina C., Willmer, Christopher N. A., Willott, Chris, and Witstok, Joris
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
Reionization is thought to be driven by faint star-forming galaxies, but characterizing this population has long remained very challenging. Here we utilize deep nine-band NIRCam imaging from JADES to study the star-forming and ionizing properties of 756 $z\sim6-9$ galaxies, including hundreds of very UV-faint objects ($M_\mathrm{UV}>-18$). The faintest ($m\sim30$) galaxies in our sample typically have stellar masses of $M_\ast\sim(1-3)\times10^7$ $M_\odot$ and young light-weighted ages ($\sim$50 Myr), though some show strong Balmer breaks implying much older ages ($\sim$500 Myr). We find no evidence for extremely massive galaxies ($>3\times10^{10}$ $M_\odot$). We infer a strong (factor $>$2) decline in the typical [OIII]$+$H$\beta$ EWs towards very faint $z\sim6-9$ galaxies, yet a weak UV luminosity dependence on the H$\alpha$ EWs at $z\sim6$. We demonstrate that these EW trends can be explained if fainter galaxies have systematically lower metallicities as well as more recently-declining star formation histories relative to the most UV-luminous galaxies in our sample. Our data provide evidence that the brightest galaxies are frequently experiencing a recent strong upturn in SFR. We also discuss how the EW trends may be influenced by a strong correlation between $M_\mathrm{UV}$ and Lyman continuum escape fraction. This alternative explanation has dramatically different implications for the contribution of galaxies along the luminosity function to cosmic reionization. Finally, we quantify the photometric overdensities around two $z>7$ strong Ly$\alpha$ emitters. One Ly$\alpha$ emitter lies close to a strong photometric overdensity while the other shows no significant nearby overdensity, perhaps implying that not all strong $z>7$ Ly$\alpha$ emitters reside in large ionized bubbles., Comment: Accepted for publication in MNRAS. Minor changes relative to previous version. Catalog of galaxy coordinates, inferred properties, and photometry available here: https://www.ryan-endsley.com/z6to9-jades-galaxy-catalog
- Published
- 2023
149. Inside the bubble: exploring the environments of reionisation-era Lyman-$\alpha$ emitting galaxies with JADES and FRESCO
- Author
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Witstok, Joris, Smit, Renske, Saxena, Aayush, Jones, Gareth C., Helton, Jakob M., Sun, Fengwu, Maiolino, Roberto, Kumari, Nimisha, Stark, Daniel P., Bunker, Andrew J., Arribas, Santiago, Baker, William M., Bhatawdekar, Rachana, Boyett, Kristan, Cameron, Alex J., Carniani, Stefano, Charlot, Stephane, Chevallard, Jacopo, Curti, Mirko, Curtis-Lake, Emma, Eisenstein, Daniel J., Endsley, Ryan, Hainline, Kevin, Ji, Zhiyuan, Johnson, Benjamin D., Looser, Tobias J., Nelson, Erica, Perna, Michele, Rix, Hans-Walter, Robertson, Brant E., Sandles, Lester, Scholtz, Jan, Simmonds, Charlotte, Tacchella, Sandro, Übler, Hannah, Williams, Christina C., Willmer, Christopher N. A., and Willott, Chris
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
We present a study of the environments of 17 Lyman-$\alpha$ (Ly$\alpha$) emitting galaxies (LAEs) in the reionisation era ($5.8 < z < 8$) identified by JWST/NIRSpec as part of the JWST Advanced Deep Extragalactic Survey (JADES). Unless situated in sufficiently (re)ionised regions, Ly$\alpha$ emission from these galaxies would be strongly absorbed by neutral gas in the intergalactic medium (IGM). We conservatively estimate sizes of the ionised regions required to reconcile the relatively low Ly$\alpha$ velocity offsets ($\Delta v_\text{Ly$\alpha$}<300\,\mathrm{km\,s^{-1}}$) with moderately high Ly$\alpha$ escape fractions ($f_\mathrm{esc,\,Ly\alpha}>5\%$) observed in our sample of LAEs, suggesting the presence of ionised hydrogen along the line of sight towards at least eight out of 17 LAEs. We find minimum physical `bubble' sizes of the order of $R_\text{ion}\sim0.1$-$1\,\mathrm{pMpc}$ are required in a patchy reionisation scenario where ionised bubbles containing the LAEs are embedded in a fully neutral IGM. Around half of the LAEs in our sample are found to coincide with large-scale galaxy overdensities seen in FRESCO at $z \sim 5.8$-$5.9$ and $z\sim7.3$, suggesting Ly$\alpha$ transmission is strongly enhanced in such overdense regions, and underlining the importance of LAEs as tracers of the first large-scale ionised bubbles. Considering only spectroscopically confirmed galaxies, we find our sample of UV-faint LAEs ($M_\text{UV}\gtrsim-20\,\mathrm{mag}$) and their direct neighbours are generally not able to produce the required ionised regions based on the Ly$\alpha$ transmission properties, suggesting lower-luminosity sources likely play an important role in carving out these bubbles. These observations demonstrate the combined power of JWST multi-object and slitless spectroscopy in acquiring a unique view of the early Universe during cosmic reionisation via the most distant LAEs., Comment: 15 pages, 8 figures. Accepted for publication in A&A
- Published
- 2023
150. JADES: The production and escape of ionizing photons from faint Lyman-alpha emitters in the epoch of reionization
- Author
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Saxena, Aayush, Bunker, Andrew J., Jones, Gareth C., Stark, Daniel P., Cameron, Alex J., Witstok, Joris, Arribas, Santiago, Baker, William M., Baum, Stefi, Bhatawdekar, Rachana, Bowler, Rebecca, Boyett, Kristan, Carniani, Stefano, Charlot, Stephane, Chevallard, Jacopo, Curti, Mirko, Curtis-Lake, Emma, Eisenstein, Daniel J., Endsley, Ryan, Hainline, Kevin, Helton, Jakob M., Johnson, Benjamin D., Kumari, Nimisha, Looser, Tobias J., Maiolino, Roberto, Rieke, Marcia, Rix, Hans-Walter, Robertson, Brant E., Sandles, Lester, Simmonds, Charlotte, Smit, Renske, Tacchella, Sandro, Williams, Christina C., Willmer, Christopher N. A., and Willott, Chris
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
We present the properties of 17 faint Ly$\alpha$ emitting galaxies (LAEs) at $z>5.8$ from the JWST Advanced Deep Extragalactic Survey (JADES) in the Hubble Ultra Deep Field/GOODS-S. These LAEs span a redshift range $z\approx5.8-8.0$ and a UV magnitude range $M_{UV}\approx-17$ to $-20.6$, with the Ly$\alpha$ equivalent width (EW) in the range $\approx 25-350$ \AA. The detection of other rest-optical emission lines in the spectra of these LAEs enables the determination of accurate systemic redshifts and Ly{\alpha} velocity offsets, as well as the physical and chemical composition of their stars and interstellar media. These faint LAEs are consistent with metal-poor systems with high ionization parameters, similar to the general galaxy population at $z>6$. We measured an average ionizing photon production efficiency, log($\xi_\rm{ion}$/erg$^{-1}$ Hz) $\approx25.57$ across our LAEs, which does not evolve strongly with redshift. We report an anti-correlation between the Ly$\alpha$ escape fraction (f_\rm{esc}) and the velocity offset from systemic redshift, consistent with model expectations. We further find that the strength and velocity offset of Ly$\alpha$ are neither correlated with galaxy spectroscopic properties nor with $\xi_\rm{ion}$. We find a decrease in $f_\rm{esc}$(Ly$\alpha$) with redshift, indicative of decreasing sizes of ionized bubbles around LAEs at high redshifts. We used a range of galaxy properties to predict Lyman continuum $f_\rm{esc}$ for our LAEs, finding that the ionizing photon output into the intergalactic medium remains roughly constant across the observed Ly$\alpha$ EW, showing a mild increase at fainter M$_{UV}$ and at higher redshifts. We derived correlations between the ionizing photon output from LAEs and $M_{UV}$, Ly$\alpha$ EW and redshifts, which can be used to constrain the ionizing photon contribution of LAEs at $z > 6$ towards cosmic reionization., Comment: Accepted for publication in A&A. 24 pages, 13 figures, spectra presented in the appendix. This updated version includes the addition of one more LAE to the sample, ID 004296 at z=6.712
- Published
- 2023
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