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158 results on '"Maccarone, T.J."'

1. Introducing the CTA concept

Author

Acharya, B.S., Actis, M., Aghajani, T., Agnetta, G., Aguilar, J., Aharonian, F., Ajello, M., Akhperjanian, A., Alcubierre, M., Aleksić, J., Alfaro, R., Aliu, E., Allafort, A.J., Allan, D., Allekotte, I., Amato, E., Anderson, J., Angüner, E.O., Antonelli, L.A., Antoranz, P., Aravantinos, A., Arlen, T., Armstrong, T., Arnaldi, H., Arrabito, L., Asano, K., Ashton, T., Asorey, H.G., Awane, Y., Baba, H., Babic, A., Baby, N., Bähr, J., Bais, A., Baixeras, C., Bajtlik, S., Balbo, M., Balis, D., Balkowski, C., Bamba, A., Bandiera, R., Barber, A., Barbier, C., Barceló, M., Barnacka, A., Barnstedt, J., Barres de Almeida, U., Barrio, J.A., Basili, A., Basso, S., Bastieri, D., Bauer, C., Baushev, A., Becerra, J., Becherini, Y., Bechtol, K.C., Becker Tjus, J., Beckmann, V., Bednarek, W., Behera, B., Belluso, M., Benbow, W., Berdugo, J., Berger, K., Bernard, F., Bernardino, T., Bernlöhr, K., Bhat, N., Bhattacharyya, S., Bigongiari, C., Biland, A., Billotta, S., Bird, T., Birsin, E., Bissaldi, E., Biteau, J., Bitossi, M., Blake, S., Blanch Bigas, O., Blasi, P., Bobkov, A., Boccone, V., Boettcher, M., Bogacz, L., Bogart, J., Bogdan, M., Boisson, C., Boix Gargallo, J., Bolmont, J., Bonanno, G., Bonardi, A., Bonev, T., Bonifacio, P., Bonnoli, G., Bordas, P., Borgland, A., Borkowski, J., Bose, R., Botner, O., Bottani, A., Bouchet, L., Bourgeat, M., Boutonnet, C., Bouvier, A., Brau-Nogué, S., Braun, I., Bretz, T., Briggs, M., Bringmann, T., Brook, P., Brun, P., Brunetti, L., Buanes, T., Buckley, J., Buehler, R., Bugaev, V., Bulgarelli, A., Bulik, T., Busetto, G., Buson, S., Byrum, K., Cailles, M., Cameron, R., Camprecios, J., Canestrari, R., Cantu, S., Capalbi, M., Caraveo, P., Carmona, E., Carosi, A., Carr, J., Carton, P.-H., Casanova, S., Casiraghi, M., Catalano, O., Cavazzani, S., Cazaux, S., Cerruti, M., Chabanne, E., Chadwick, P., Champion, C., Chen, A., Chiang, J., Chiappetti, L., Chikawa, M., Chitnis, V.R., Chollet, F., Chudoba, J., Cieślar, M., Cillis, A., Cohen-Tanugi, J., Colafrancesco, S., Colin, P., Colome, J., Colonges, S., Compin, M., Conconi, P., Conforti, V., Connaughton, V., Conrad, J., Contreras, J.L., Coppi, P., Corona, P., Corti, D., Cortina, J., Cossio, L., Costantini, H., Cotter, G., Courty, B., Couturier, S., Covino, S., Crimi, G., Criswell, S.J., Croston, J., Cusumano, G., Dafonseca, M., Dale, O., Daniel, M., Darling, J., Davids, I., Dazzi, F., De Angelis, A., De Caprio, V., De Frondat, F., de Gouveia Dal Pino, E.M., de la Calle, I., De La Vega, G.A., de los Reyes Lopez, R., De Lotto, B., De Luca, A., de Mello Neto, J.R.T., de Naurois, M., de Oliveira, Y., de Oña Wilhelmi, E., de Souza, V., Decerprit, G., Decock, G., Deil, C., Delagnes, E., Deleglise, G., Delgado, C., Della Volpe, D., Demange, P., Depaola, G., Dettlaff, A., Di Paola, A., Di Pierro, F., Díaz, C., Dick, J., Dickherber, R., Dickinson, H., Diez-Blanco, V., Digel, S., Dimitrov, D., Disset, G., Djannati-Ataï, A., Doert, M., Dohmke, M., Domainko, W., Dominis Prester, D., Donat, A., Dorner, D., Doro, M., Dournaux, J.-L., Drake, G., Dravins, D., Drury, L., Dubois, F., Dubois, R., Dubus, G., Dufour, C., Dumas, D., Dumm, J., Durand, D., Dyks, J., Dyrda, M., Ebr, J., Edy, E., Egberts, K., Eger, P., Einecke, S., Eleftheriadis, C., Elles, S., Emmanoulopoulos, D., Engelhaupt, D., Enomoto, R., Ernenwein, J.-P., Errando, M., Etchegoyen, A., Evans, P., Falcone, A., Fantinel, D., Farakos, K., Farnier, C., Fasola, G., Favill, B., Fede, E., Federici, S., Fegan, S., Feinstein, F., Ferenc, D., Ferrando, P., Fesquet, M., Fiasson, A., Fillin-Martino, E., Fink, D., Finley, C., Finley, J.P., Fiorini, M., Firpo Curcoll, R., Flores, H., Florin, D., Focke, W., Föhr, C., Fokitis, E., Font, L., Fontaine, G., Fornasa, M., Förster, A., Fortson, L., Fouque, N., Franckowiak, A., Fransson, C., Fraser, G., Frei, R., Albuquerque, I.F.M., Fresnillo, L., Fruck, C., Fujita, Y., Fukazawa, Y., Fukui, Y., Funk, S., Gäbele, W., Gabici, S., Gabriele, R., Gadola, A., Galante, N., Gall, D., Gallant, Y., Gámez-García, J., García, B., Garcia López, R., Gardiol, D., Garrido, D., Garrido, L., Gascon, D., Gaug, M., Gaweda, J., Gebremedhin, L., Geffroy, N., Gerard, L., Ghedina, A., Ghigo, M., Giannakaki, E., Gianotti, F., Giarrusso, S., Giavitto, G., Giebels, B., Gika, V., Giommi, P., Girard, N., Giro, E., Giuliani, A., Glanzman, T., Glicenstein, J.-F., Godinovic, N., Golev, V., Gomez Berisso, M., Gómez-Ortega, J., Gonzalez, M.M., González, A., González, F., González Muñoz, A., Gothe, K.S., Gougerot, M., Graciani, R., Grandi, P., Grañena, F., Granot, J., Grasseau, G., Gredig, R., Green, A., Greenshaw, T., Grégoire, T., Grimm, O., Grube, J., Grudzinska, M., Gruev, V., Grünewald, S., Grygorczuk, J., Guarino, V., Gunji, S., Gyuk, G., Hadasch, D., Hagiwara, R., Hahn, J., Hakansson, N., Hallgren, A., Hamer Heras, N., Hara, S., Hardcastle, M.J., Harris, J., Hassan, T., Hatanaka, K., Haubold, T., Haupt, A., Hayakawa, T., Hayashida, M., Heller, R., Henault, F., Henri, G., Hermann, G., Hermel, R., Herrero, A., Hidaka, N., Hinton, J., Hoffmann, D., Hofmann, W., Hofverberg, P., Holder, J., Horns, D., Horville, D., Houles, J., Hrabovsky, M., Hrupec, D., Huan, H., Huber, B., Huet, J.-M., Hughes, G., Humensky, T.B., Huovelin, J., Ibarra, A., Illa, J.M., Impiombato, D., Incorvaia, S., Inoue, S., Inoue, Y., Ioka, K., Ismailova, E., Jablonski, C., Jacholkowska, A., Jamrozy, M., Janiak, M., Jean, P., Jeanney, C., Jimenez, J.J., Jogler, T., Johnson, T., Journet, L., Juffroy, C., Jung, I., Kaaret, P., Kabuki, S., Kagaya, M., Kakuwa, J., Kalkuhl, C., Kankanyan, R., Karastergiou, A., Kärcher, K., Karczewski, M., Karkar, S., Kasperek, J., Kastana, D., Katagiri, H., Kataoka, J., Katarzyński, K., Katz, U., Kawanaka, N., Kellner-Leidel, B., Kelly, H., Kendziorra, E., Khélifi, B., Kieda, D.B., Kifune, T., Kihm, T., Kishimoto, T., Kitamoto, K., Kluźniak, W., Knapic, C., Knapp, J., Knödlseder, J., Köck, F., Kocot, J., Kodani, K., Köhne, J.-H., Kohri, K., Kokkotas, K., Kolitzus, D., Komin, N., Kominis, I., Konno, Y., Köppel, H., Korohoda, P., Kosack, K., Koss, G., Kossakowski, R., Kostka, P., Koul, R., Kowal, G., Koyama, S., Kozioł, J., Krähenbühl, T., Krause, J., Krawzcynski, H., Krennrich, F., Krepps, A., Kretzschmann, A., Krobot, R., Krueger, P., Kubo, H., Kudryavtsev, V.A., Kushida, J., Kuznetsov, A., La Barbera, A., La Palombara, N., La Parola, V., La Rosa, G., Lacombe, K., Lamanna, G., Lande, J., Languignon, D., Lapington, J., Laporte, P., Lavalley, C., Le Flour, T., Le Padellec, A., Lee, S.-H., Lee, W.H., Leigui de Oliveira, M.A., Lelas, D., Lenain, J.-P., Leopold, D.J., Lerch, T., Lessio, L., Lieunard, B., Lindfors, E., Liolios, A., Lipniacka, A., Lockart, H., Lohse, T., Lombardi, S., Lopatin, A., Lopez, M., López-Coto, R., López-Oramas, A., Lorca, A., Lorenz, E., Lubinski, P., Lucarelli, F., Lüdecke, H., Ludwin, J., Luque-Escamilla, P.L., Lustermann, W., Luz, O., Lyard, E., Maccarone, M.C., Maccarone, T.J., Madejski, G.M., Madhavan, A., Mahabir, M., Maier, G., Majumdar, P., Malaguti, G., Maltezos, S., Manalaysay, A., Mancilla, A., Mandat, D., Maneva, G., Mangano, A., Manigot, P., Mannheim, K., Manthos, I., Maragos, N., Marcowith, A., Mariotti, M., Marisaldi, M., Markoff, S., Marszałek, A., Martens, C., Martí, J., Martin, J.-M., Martin, P., Martínez, G., Martínez, F., Martínez, M., Masserot, A., Mastichiadis, A., Mathieu, A., Matsumoto, H., Mattana, F., Mattiazzo, S., Maurin, G., Maxfield, S., Maya, J., Mazin, D., Mc Comb, L., McCubbin, N., McHardy, I., McKay, R., Medina, C., Melioli, C., Melkumyan, D., Mereghetti, S., Mertsch, P., Meucci, M., Michałowski, J., Micolon, P., Mihailidis, A., Mineo, T., Minuti, M., Mirabal, N., Mirabel, F., Miranda, J.M., Mirzoyan, R., Mizuno, T., Moal, B., Moderski, R., Mognet, I., Molinari, E., Molinaro, M., Montaruli, T., Monteiro, I., Moore, P., Moralejo Olaizola, A., Mordalska, M., Morello, C., Mori, K., Mottez, F., Moudden, Y., Moulin, E., Mrusek, I., Mukherjee, R., Munar-Adrover, P., Muraishi, H., Murase, K., Murphy, A., Nagataki, S., Naito, T., Nakajima, D., Nakamori, T., Nakayama, K., Naumann, C., Naumann, D., Naumann-Godo, M., Nayman, P., Nedbal, D., Neise, D., Nellen, L., Neustroev, V., Neyroud, N., Nicastro, L., Nicolau-Kukliński, J., Niedźwiecki, A., Niemiec, J., Nieto, D., Nikolaidis, A., Nishijima, K., Nolan, S., Northrop, R., Nosek, D., Nowak, N., Nozato, A., O’Brien, P., Ohira, Y., Ohishi, M., Ohm, S., Ohoka, H., Okuda, T., Okumura, A., Olive, J.-F., Ong, R.A., Orito, R., Orr, M., Osborne, J., Ostrowski, M., Otero, L.A., Otte, N., Ovcharov, E., Oya, I., Ozieblo, A., Padilla, L., Paiano, S., Paillot, D., Paizis, A., Palanque, S., Palatka, M., Pallota, J., Panagiotidis, K., Panazol, J.-L., Paneque, D., Panter, M., Paoletti, R., Papayannis, A., Papyan, G., Paredes, J.M., Pareschi, G., Parks, G., Parraud, J.-M., Parsons, D., Paz Arribas, M., Pech, M., Pedaletti, G., Pelassa, V., Pelat, D., Perez, M.d.C., Persic, M., Petrucci, P.-O., Peyaud, B., Pichel, A., Pita, S., Pizzolato, F., Platos, Ł., Platzer, R., Pogosyan, L., Pohl, M., Pojmanski, G., Ponz, J.D., Potter, W., Poutanen, J., Prandini, E., Prast, J., Preece, R., Profeti, F., Prokoph, H., Prouza, M., Proyetti, M., Puerto-Gimenez, I., Pühlhofer, G., Puljak, I., Punch, M., Pyzioł, R., Quel, E.J., Quinn, J., Quirrenbach, A., Racero, E., Rajda, P.J., Ramon, P., Rando, R., Rannot, R.C., Rataj, M., Raue, M., Reardon, P., Reimann, O., Reimer, A., Reimer, O., Reitberger, K., Renaud, M., Renner, S., Reville, B., Rhode, W., Ribó, M., Ribordy, M., Richer, M.G., Rico, J., Ridky, J., Rieger, F., Ringegni, P., Ripken, J., Ristori, P.R., Riviére, A., Rivoire, S., Rob, L., Roeser, U., Rohlfs, R., Rojas, G., Romano, P., Romaszkan, W., Romero, G.E., Rosen, S., Rosier Lees, S., Ross, D., Rouaix, G., Rousselle, J., Rousselle, S., Rovero, A.C., Roy, F., Royer, S., Rudak, B., Rulten, C., Rupiński, M., Russo, F., Ryde, F., Sacco, B., Saemann, E.O., Saggion, A., Sahakian, V., Saito, K., Saito, T., Saito, Y., Sakaki, N., Sakonaka, R., Salini, A., Sanchez, F., Sanchez-Conde, M., Sandoval, A., Sandaker, H., Sant’Ambrogio, E., Santangelo, A., Santos, E.M., Sanuy, A., Sapozhnikov, L., Sarkar, S., Sartore, N., Sasaki, H., Satalecka, K., Sawada, M., Scalzotto, V., Scapin, V., Scarcioffolo, M., Schafer, J., Schanz, T., Schlenstedt, S., Schlickeiser, R., Schmidt, T., Schmoll, J., Schovanek, P., Schroedter, M., Schultz, C., Schultze, J., Schulz, A., Schure, K., Schwab, T., Schwanke, U., Schwarz, J., Schwarzburg, S., Schweizer, T., Schwemmer, S., Segreto, A., Seiradakis, J.-H., Sembroski, G.H., Seweryn, K., Sharma, M., Shayduk, M., Shellard, R.C., Shi, J., Shibata, T., Shibuya, A., Shum, E., Sidoli, L., Sidz, M., Sieiro, J., Sikora, M., Silk, J., Sillanpää, A., Singh, B.B., Sitarek, J., Skole, C., Smareglia, R., Smith, A., Smith, D., Smith, J., Smith, N., Sobczyńska, D., Sol, H., Sottile, G., Sowiński, M., Spanier, F., Spiga, D., Spyrou, S., Stamatescu, V., Stamerra, A., Starling, R., Stawarz, Ł., Steenkamp, R., Stegmann, C., Steiner, S., Stergioulas, N., Sternberger, R., Sterzel, M., Stinzing, F., Stodulski, M., Straumann, U., Strazzeri, E., Stringhetti, L., Suarez, A., Suchenek, M., Sugawara, R., Sulanke, K.-H., Sun, S., Supanitsky, A.D., Suric, T., Sutcliffe, P., Sykes, J., Szanecki, M., Szepieniec, T., Szostek, A., Tagliaferri, G., Tajima, H., Takahashi, H., Takahashi, K., Takalo, L., Takami, H., Talbot, G., Tammi, J., Tanaka, M., Tanaka, S., Tasan, J., Tavani, M., Tavernet, J.-P., Tejedor, L.A., Telezhinsky, I., Temnikov, P., Tenzer, C., Terada, Y., Terrier, R., Teshima, M., Testa, V., Tezier, D., Thuermann, D., Tibaldo, L., Tibolla, O., Tiengo, A., Tluczykont, M., Todero Peixoto, C.J., Tokanai, F., Tokarz, M., Toma, K., Torii, K., Tornikoski, M., Torres, D.F., Torres, M., Tosti, G., Totani, T., Toussenel, F., Tovmassian, G., Travnicek, P., Trifoglio, M., Troyano, I., Tsinganos, K., Ueno, H., Umehara, K., Upadhya, S.S., Usher, T., Uslenghi, M., Valdes-Galicia, J.F., Vallania, P., Vallejo, G., van Driel, W., van Eldik, C., Vandenbrouke, J., Vanderwalt, J., Vankov, H., Vasileiadis, G., Vassiliev, V., Veberic, D., Vegas, I., Vercellone, S., Vergani, S., Veyssiére, C., Vialle, J.P., Viana, A., Videla, M., Vincent, P., Vincent, S., Vink, J., Vlahakis, N., Vlahos, L., Vogler, P., Vollhardt, A., von Gunten, H.-P., Vorobiov, S., Vuerli, C., Waegebaert, V., Wagner, R., Wagner, R.G., Wagner, S., Wakely, S.P., Walter, R., Walther, T., Warda, K., Warwick, R., Wawer, P., Wawrzaszek, R., Webb, N., Wegner, P., Weinstein, A., Weitzel, Q., Welsing, R., Werner, M., Wetteskind, H., White, R., Wierzcholska, A., Wiesand, S., Wilkinson, M., Williams, D.A., Willingale, R., Winiarski, K., Wischnewski, R., Wiśniewski, Ł., Wood, M., Wörnlein, A., Xiong, Q., Yadav, K.K., Yamamoto, H., Yamamoto, T., Yamazaki, R., Yanagita, S., Yebras, J.M., Yelos, D., Yoshida, A., Yoshida, T., Yoshikoshi, T., Zabalza, V., Zacharias, M., Zajczyk, A., Zanin, R., Zdziarski, A., Zech, A., Zhao, A., Zhou, X., Ziętara, K., Ziolkowski, J., Ziółkowski, P., Zitelli, V., Zurbach, C., and Żychowski, P.

Published
2013
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2. Identification of the Hard X-Ray Source Dominating the E > 25 keV Emission of the Nearby Galaxy M31

Author

Yukita, M, Ptak, A, Hornschemeier, A. E, Wik, D, Maccarone, T.J, Pottschmidt, Katja, Zezas, A, Antoniou, V, Ballhausen, R, Lehmer, B.D, and Boyd, P. T

Subjects
Astrophysics
Abstract

We report the identification of a bright hard X-ray source dominating the M31 bulge above 25 kiloelectronvolts from a simultaneous NuSTAR-Swift observation. We find that this source is the counterpart to Swift J0042.6+4112, which was previously detected in the Swift BAT All-Sky Hard X-Ray Survey. This Swift BAT source had been suggested to be the combined emission from a number of point sources; our new observations have identified a single X-ray source from 0.5 to 50 kiloelectronvolts as the counterpart for the first time. In the 0.5-10 kiloelectronvolt band, the source had been classified as an X-ray Binary candidate in various Chandra and XMM-Newton studies; however, since it was not clearly associated with Swift J0042.6+4112, the previous E is less than 10 kiloelectronvolts observations did not generate much attention. This source has a spectrum with a soft X-ray excess (kT approximately equal to 0.2 kiloelectronvolts) plus a hard spectrum with a power law of gamma approximately equal to 1 and a cutoff around 15-20 kiloelectronvolts, typical of the spectral characteristics of accreting pulsars. Unfortunately, any potential pulsation was undetected in the NuSTAR data, possibly due to insufficient photon statistics. The existing deep HST (Hubble Space Telescope) images exclude high-mass (greater than 3 times the radius of the moon) donors at the location of this source. The best interpretation for the nature of this source is an X-ray pulsar with an intermediate-mass (less than 3 times the radius of the moon M) companion or a symbiotic X-ray binary. We discuss other possibilities in more detail.

Published
2017
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3. Swift Bulge Survey: Discovery of a new X-ray transient, Swift J174038.1-273712

Author

Bahramian, A., Heinke, C.O., Maccarone, T.J., Shaw, A.W., Wijnands, R., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Computer Science::Digital Libraries, Astrophysics::Galaxy Astrophysics
Abstract

The Swift Bulge Survey performs biweekly mapping of 16 square degrees of the Galactic Bulge with short (~120 s) X-ray observations (Shaw et al.2020, MNRAS, 492, 4344; Bahramian et al. 2021, MNRAS, 501, 2790).

Published
2021

4. Dynamical modelling of CXOGBS J175553.2−281633: a 10 h long orbital period cataclysmic variable

Author

Gomez, S., Perez Torres, M.A., Jonker, P.G., Kostrzewa-Rutkowska, Z.P., Grunsven, T.F.J. van, Udalski, A., Hynes, R.I., Heinke, C.O., Maccarone, T.J., Salinas, R., Strader, J., Gomez, S., Perez Torres, M.A., Jonker, P.G., Kostrzewa-Rutkowska, Z.P., Grunsven, T.F.J. van, Udalski, A., Hynes, R.I., Heinke, C.O., Maccarone, T.J., Salinas, R., and Strader, J.

Abstract

Contains fulltext : 230763.pdf (publisher's version ) (Open Access)

Published
2021

5. LeMMINGs III. The e-MERLIN legacy survey of the Palomar sample: exploring the origin of nuclear radio emission in active and inactive galaxies through the [O iii] – radio connection

Author

Baldi, R.D., Williams, D.R.A., Beswick, R.J., McHardy, I., Dullo, B.T., Knapen, J.H., Zanisi, L., Argo, M.K., Aalto, S., Alberdi, A., Baan, W.A., Bendo, G.J., Fenech, D.M., Green, D.A., Klöckner, H.-R., Körding, E., Maccarone, T.J., Marcaide, J.M., Mutie, I., Panessa, F., Pérez-Torres, M.A., Romero-Cañizales, C., Saikia, D.J., Saikia, P., Shankar, F., Spencer, R.E., Stevens, I.R., Uttley, P., Brinks, E., Corbel, S., Martí-Vidal, I., Mundell, C.G., Pahari, M., Ward, M.J., Baldi, R.D., Williams, D.R.A., Beswick, R.J., McHardy, I., Dullo, B.T., Knapen, J.H., Zanisi, L., Argo, M.K., Aalto, S., Alberdi, A., Baan, W.A., Bendo, G.J., Fenech, D.M., Green, D.A., Klöckner, H.-R., Körding, E., Maccarone, T.J., Marcaide, J.M., Mutie, I., Panessa, F., Pérez-Torres, M.A., Romero-Cañizales, C., Saikia, D.J., Saikia, P., Shankar, F., Spencer, R.E., Stevens, I.R., Uttley, P., Brinks, E., Corbel, S., Martí-Vidal, I., Mundell, C.G., Pahari, M., and Ward, M.J.

Abstract

Contains fulltext : 239375.pdf (Publisher’s version ) (Open Access)

Published
2021

6. X-ray observations of two candidate symbiotic binaries in the galactic bulge

Author

Wetuski, J., Hynes, R.I., Maccarone, T.J., Heinke, C., Torres, M.A.P., Jonker, P.G., Britt, C.T., Steeghs, D., Nelemans, G., Wetuski, J., Hynes, R.I., Maccarone, T.J., Heinke, C., Torres, M.A.P., Jonker, P.G., Britt, C.T., Steeghs, D., and Nelemans, G.

Abstract

Contains fulltext : 236335.pdf (Publisher’s version ) (Open Access)

Published
2021

7. Cygnus X-1 contains a 21-solar mass black hole-Implications for massive star winds

Author

Miller-Jones, James, Bahramian, Arash, Orosz, J.A., Mande, I., Gou, L., Maccarone, T.J., Neijsse, C.J., Zhao, X., Ziółkowski, J., Reid, M.J., Uttley, P., Zheng, X., Byun, D.Y., Dodson, R., Grinberg, V., Jung, T., Kim, J.S., Marcote, B., Markoff, S., Rioja, M.J., Rushton, A.P., Russell, D.M., Sivakoff, G.R., Tetarenko, A.J., Tudose, V., Wilms, J., Miller-Jones, James, Bahramian, Arash, Orosz, J.A., Mande, I., Gou, L., Maccarone, T.J., Neijsse, C.J., Zhao, X., Ziółkowski, J., Reid, M.J., Uttley, P., Zheng, X., Byun, D.Y., Dodson, R., Grinberg, V., Jung, T., Kim, J.S., Marcote, B., Markoff, S., Rioja, M.J., Rushton, A.P., Russell, D.M., Sivakoff, G.R., Tetarenko, A.J., Tudose, V., and Wilms, J.

Abstract

The evolution of massive stars is influenced by the mass lost to stellar winds over their lifetimes. These winds limit the masses of the stellar remnants (such as black holes) that the stars ultimately produce. We used radio astrometry to refine the distance to the black hole X-ray binary Cygnus X-1, which we found to be 2:220:180:17 kiloparsecs. When combined with archival optical data, this implies a black hole mass of 21.2 ± 2.2 solar masses, which is higher than previous measurements. The formation of such a high-mass black hole in a high-metallicity system (within the Milky Way) constrains wind mass loss from massive stars.

Published
2021

8. Towards a larger sample of radio jets from quiescent black hole X-ray binaries

Author

Plotkin, Richard, Bahramian, Arash, Miller-Jones, James, Reynolds, M.T., Atri, P., Maccarone, T.J., Shaw, A.W., Gandhi, P., Plotkin, Richard, Bahramian, Arash, Miller-Jones, James, Reynolds, M.T., Atri, P., Maccarone, T.J., Shaw, A.W., and Gandhi, P.

Abstract

Quiescent black hole X-ray binaries (X-ray luminosities ≲1034 erg s−1) are believed to be fed by hot accretion flows that launch compact, relativistic jets. However, due to their low luminosities, quiescent jets have been detected in the radio waveband from only five systems so far. Here, we present radio observations of two quiescent black hole X-ray binaries with the Australia Telescope Compact Array. One system, GS 1124-684, was not detected. The other system, BW Cir, was detected over two different epochs in 2018 and 2020, for which we also obtained quasi-simultaneous X-ray detections with Chandra and Swift. BW Cir is now the sixth quiescent X-ray binary with a confirmed radio jet. However, the distance to BW Cir is uncertain, and we find that BW Cir shows different behaviour in the radio/X-ray luminosity plane depending on the correct distance. Estimates based on its G-type subgiant donor star place BW Cir at >25 kpc, while initial optical astrometric measurements from Gaia Data Release 2 suggested likely distances of just a few kpc. Here, we use the most recent measurements from Gaia Early Data Release 3 and find a distance d = 7.1+4.8−3.9 kpc and a potential kick velocity PKV = 165+81−17 km s−1, with distances up to ≈20 kpc possible based on its parallax and proper motion. Even though there is now less tension between the parallax and donor-star based distance measurements, it remains an unresolved matter, and we conclude with suggestions on how to reconcile the two measurements.

Published
2021

9. Wind Mass-loss Rates of Stripped Stars Inferred from Cygnus X-1

Author

Neijssel, C.J., Vinciguerra, S., Vigna-Gómez, A., Hirai, R., Miller-Jones, James, Bahramian, Arash, Maccarone, T.J., Mandel, I., Neijssel, C.J., Vinciguerra, S., Vigna-Gómez, A., Hirai, R., Miller-Jones, James, Bahramian, Arash, Maccarone, T.J., and Mandel, I.

Abstract

Recent observations of the high-mass X-ray binary Cygnus X-1 have shown that both the companion star (41 solar masses) and the black hole (21 solar masses) are more massive than previously estimated. Furthermore, the black hole appears to be nearly maximally spinning. Here, we present a possible formation channel for the Cygnus X-1 system that matches the observed system properties. In this formation channel, we find that the orbital parameters of Cygnus X-1, combined with the observed metallicity of the companion, imply a significant reduction in mass loss through winds relative to commonly used prescriptions for stripped stars.

Published
2021

10. Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070

Author

Tetarenko, A.J., Casella, P., Miller-Jones, James, Sivakoff, G.R., Paice, J.A., Vincentelli, F.M., Maccarone, T.J., Gandhi, P., Dhillon, V.S., Marsh, T.R., Russell, T.D., Uttley, P., Tetarenko, A.J., Casella, P., Miller-Jones, James, Sivakoff, G.R., Paice, J.A., Vincentelli, F.M., Maccarone, T.J., Gandhi, P., Dhillon, V.S., Marsh, T.R., Russell, T.D., and Uttley, P.

Abstract

We present multiwavelength fast timing observations of the black hole X-ray binary MAXI J1820+070 (ASASSN-18ey), taken with the Karl G. Jansky Very Large Array (VLA), Atacama Large Millimeter/Sub-Millimeter Array (ALMA), Very Large Telescope (VLT), New Technology Telescope (NTT), Neutron Star Interior Composition Explorer (NICER), and XMM-Newton. Our data set simultaneously samples 10 different electromagnetic bands (radio - X-ray) over a 7-h period during the hard state of the 2018-2019 outburst. The emission we observe is highly variable, displaying multiple rapid flaring episodes. To characterize the variability properties in our data, we implemented a combination of cross-correlation and Fourier analyses. We find that the emission is highly correlated between different bands, measuring time-lags ranging from hundreds of milliseconds between the X-ray/optical bands to minutes between the radio/sub-mm bands. Our Fourier analysis also revealed, for the first time in a black hole X-ray binary, an evolving power spectral shape with electromagnetic frequency. Through modelling these variability properties, we find that MAXI J1820+070 launches a highly relativistic (Gamma =6.81 +1.06 -1.15}$) and confined (phi =0.45 +0.13 -0.11 deg) jet, which is carrying a significant amount of power away from the system (equivalent to sim 0.6 , L-{1-100{rm keV}). We additionally place constraints on the jet composition and magnetic field strength in the innermost jet base region. Overall, this work demonstrates that time-domain analysis is a powerful diagnostic tool for probing jet physics, where we can accurately measure jet properties with time-domain measurements alone.

Published
2021

11. An extremely luminous X-ray outburst at the birth of a supernova

Author

Soderberg, A.M., Berger, E., Page, K.L., Schady, P., Parrent, J., Pooley, D., Wang, X.-Y., Ofek, E.O., Cucchiara, A., Rau, A., Waxman, E., Simon, J.D., Bock, D.C.-J., Milne, P.A., Page, M.J., Barentine, J.C., Barthelmy, S.D., Beardmore, A.P., Bietenholz, M.F., Brown, P., Burrows, A., Burrows, D.N., Byrngelson, G., Cenko, S.B., Chandra, P., Cummings, J.R., Fox, D.B., Gal-Yam, A., Gehrels, N., Immler, S., Kasliwal, M., Kong, A.K.H., Krimm, H.A., Kulkarni, S.R., Maccarone, T.J., Meszaros, P., Nakar, E., O'Brien, P.T., Overzier, R.A., de Pasquale, M., Racusin, J., Rea, N., and York, D.G.

Subjects
Supernovae -- Observations, X-rays -- Observations, Environmental issues, Science and technology, Zoology and wildlife conservation, Observations
Abstract

Massive stars end their short lives in spectacular explosions--supernovae--that synthesize new elements and drive galaxy evolution. Historically, supernovae were discovered mainly through their 'delayed' optical light (some days after the [...]

Published
2008

12. VLA detection of a likely radio counterpart of IGR J17494-3030

Author

van den Eijnden, J., Degenaar, N., Wijnands, R., Russell, T.D., Stoop, M., Armas Padilla, M., Russell, D.M., Maitra, D., Heinke, C.O., Sivakoff, G. R., Shaw, A.W., Maccarone, T.J., Miller-Jones, J.C.A., Bahramian, A., High Energy Astrophys. & Astropart. Phys (API, FNWI), and API Other Research (FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics
Abstract

IGR J17494-3030 is a transient X-ray binary that was recently reported to be in outburst by INTEGRAL (ATel #14119). Follow-up NICER observations have subsequently shown the presence of X-ray pulsations at 376 Hz (ATel #14124), confirming the neutron star nature of the compact object and identifying IGR J17494-3030 as an accreting millisecond X-ray pulsar (AMXP).

Published
2020

13. VLA radio detection of the new X-ray transient SRGt J071522.1-191609

Author

van den Eijnden, J., Degenaar, N., Wijnands, R., Russell, T., Stoop, M., Armas Padilla, M., Russell, D.M., Maitra, D., Heinke, C.O., Sivakoff, G.R., Shaw, A.W., Maccarone, T.J., Miller-Jones, J.C.A., Bahramian, A., High Energy Astrophys. & Astropart. Phys (API, FNWI), and API Other Research (FNWI)

Abstract

Following the eROSITA discovery of the new X-ray transient SRGt J071522.1-191609 (ATel #13657) and the first follow-up observation using the X-ray telescope (XRT) on board the Neil Gehrels Swift Observatory (ATel #13661), we triggered an X-ray and radio monitoring program using Swift/XRT and the Karl G. Jansky Very Large Array (VLA).

Published
2020

14. A radio parallax to the black hole X-ray binary MAXI J1820+070

Author

Atri, P., Miller-Jones, J.C.A., Bahramian, A., Plotkin, R.M., Deller, A.T., Jonker, P.G., Maccarone, T.J., Sivakoff, G.R., Soria, R., Altamirano, D., Belloni, T., Fender, R., Körding, E., Maitra, D., Markoff, S., Migliari, S., Russell, D., Russell, T., Sarazin, C.L., Tetarenko, A.J., Tudose, V., Atri, P., Miller-Jones, J.C.A., Bahramian, A., Plotkin, R.M., Deller, A.T., Jonker, P.G., Maccarone, T.J., Sivakoff, G.R., Soria, R., Altamirano, D., Belloni, T., Fender, R., Körding, E., Maitra, D., Markoff, S., Migliari, S., Russell, D., Russell, T., Sarazin, C.L., Tetarenko, A.J., and Tudose, V.

Abstract

Contains fulltext : 216840.pdf (publisher's version ) (Open Access)

Published
2020

15. The MAVERIC survey: Chandra/ACIS catalog of faint X-ray sources in 38 galactic globular clusters

Author

Bahramian, Arash, Strader, J., Miller-Jones, James, Chomiuk, L., Heinke, C.O., Maccarone, T.J., Pooley, D., Shishkovsky, L., Tudor, V., Zhao, Y., Li, K.L., Sivakoff, G.R., Tremou, E., Buchner, J., Bahramian, Arash, Strader, J., Miller-Jones, James, Chomiuk, L., Heinke, C.O., Maccarone, T.J., Pooley, D., Shishkovsky, L., Tudor, V., Zhao, Y., Li, K.L., Sivakoff, G.R., Tremou, E., and Buchner, J.

Abstract

Globular clusters host a variety of lower-luminosity (LX < 1035 erg s−1) X-ray sources, including accreting neutron stars (NSs) and black holes (BHs), millisecond pulsars (MSPs), cataclysmic variables, and chromospherically active binaries. In this paper, we provide a comprehensive catalog of more than 1100 X-ray sources in 38 Galactic globular clusters (GCs) observed by the Chandra X-ray Observatory's Chandra/ACIS detector. The targets are selected to complement the MAVERIC survey's deep radio continuum maps of Galactic GCs. We perform photometry and spectral analysis for each source, determine a best-fit model, and assess the possibility of it being a foreground or background source based on its spectral properties and location in the cluster. We also provide basic assessments of variability. We discuss the distribution of X-ray binaries in GCs and their X-ray luminosity function, and we carefully analyze systems with LX > 1033 erg s−1. Among these moderately bright systems, we discover a new source in NGC 6539 that may be a candidate accreting stellar-mass BH or a transitional MSP. We show that quiescent NS low-mass X-ray binaries in GCs may spend ∼2% of their lifetimes as transitional MSPs in their active (LX > 1033 erg s−1) state. Finally, we identify a substantial underabundance of bright (LX > 1033 erg s−1) intermediate polars in GCs compared to the Galactic field, in contrast with the literature of the past two decades.

Published
2020

16. Nustar and Chandra Insight into the Nature of the 3-40 Kev Nuclear Emission in Ngc 253

Author

Lehmer, Bret D, Wik, Daniel R, Hornschemeier, Ann E, Ptak, Andrew, Antoniu, V, Argo, M.K, Bechtol, K, Boggs, S, Christensen, F.E, Craig, W.W, Hailey, C.J, Harrison, F.A, Krivonos, R, Leyder, Jean-Christophe Xavier Georges, Maccarone, T.J, Stern, D, Venters, T, Zezas, A, and Zhang, W.W

Subjects
Astrophysics, Astronomy
Abstract

We present results from three nearly simultaneous Nuclear Spectroscopic Telescope Array (NuSTAR) and Chandra monitoring observations between 2012 September 2 and 2012 November 16 of the local star-forming galaxy NGC 253. The 3-40 kiloelectron volt intensity of the inner approximately 20 arcsec (approximately 400 parsec) nuclear region, as measured by NuSTAR, varied by a factor of approximately 2 across the three monitoring observations. The Chandra data reveal that the nuclear region contains three bright X-ray sources, including a luminous (L (sub 2-10 kiloelectron volt) approximately few × 10 (exp 39) erg per s) point source located approximately 1 arcsec from the dynamical center of the galaxy (within the sigma 3 positional uncertainty of the dynamical center); this source drives the overall variability of the nuclear region at energies greater than or approximately equal to 3 kiloelectron volts. We make use of the variability to measure the spectra of this single hard X-ray source when it was in bright states. The spectra are well described by an absorbed (power-law model spectral fit value, N(sub H), approximately equal to 1.6 x 10 (exp 23) per square centimeter) broken power-law model with spectral slopes and break energies that are typical of ultraluminous X-ray sources (ULXs), but not active galactic nuclei (AGNs). A previous Chandra observation in 2003 showed a hard X-ray point source of similar luminosity to the 2012 source that was also near the dynamical center (Phi is approximately equal to 0.4 arcsec); however, this source was offset from the 2012 source position by approximately 1 arcsec. We show that the probability of the 2003 and 2012 hard X-ray sources being unrelated is much greater than 99.99% based on the Chandra spatial localizations. Interestingly, the Chandra spectrum of the 2003 source (3-8 kiloelectron volts) is shallower in slope than that of the 2012 hard X-ray source. Its proximity to the dynamical center and harder Chandra spectrum indicate that the 2003 source is a better AGN candidate than any of the sources detected in our 2012 campaign; however, we were unable to rule out a ULX nature for this source. Future NuSTAR and Chandra monitoring would be well equipped to break the degeneracy between the AGN and ULX nature of the 2003 source, if again caught in a high state.

Published
2013
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17. Swift Bulge Survey: X-ray activity of bursters KS 1741-293, IGR J17445-2747, SAX J1750.8-2900, and symbiotic X-ray binary XMMU J174445.5-295044

Author

Heinke, C.O., Bahramian, A., Wijnands, R., Maccarone, T.J., Degenaar, N., in't Zand, J.J.M., Kennea, J.A., Kuulkers, E., Rivera-Sandoval, L., Shaw, A.W., Sivakoff, G.R., Strader, J., Tetarenko, A.J., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

The Swift Bulge Survey performs rapid shallow mapping of 16 squaredegrees of the Galactic Bulge with short (120-s in 2019) observations(see Atels #10265,#10273,#10305,#10355,#10419,#10422,#10428,#12751). After our first 2019 observations on April 4, 18 and May 8-9, we conducted further Swift Bulge Survey observations on May 16, May 23, and May 30.

Published
2019

18. Swift Bulge Survey detections of the X-ray transients SAX J1750.8-2900 and IGR J17445-2747

Author

Heinke, C.O., Bahramian, A., Wijnands, R., Maccarone, T.J., Degenaar, N., in't Zand, J.J.M., Kennea, J.A., Kuulkers, E., Rivera-Sandoval, L., Shaw, A.W., Sivakoff, G.R., Strader, J., Tetarenko, A.J., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We have begun a second installment of our Swift Bulge Survey (Atels #10265,#10273,#10305,#10355,#10419,#10422,#10428), a rapid shallow mapping of 16 square degrees of the Galactic Bulge.

Published
2019

19. STROBE-X: X-ray Timing & Spectroscopy on Dynamical Timescales from Microseconds to Years

Author

Wilson-Hodge, C.A., Ray, P.S., Maccarone, T.J., Chakrabarty, D., Gendreau, K.C., Arzoumanian, Z., Jenke, P., Ballantyne, D., Bozzo, E., Brandt, S., Brenneman, L., Christophersen, M., DeRosa, A., Feroci, M., Goldstein, A., Hartmann, D., Hernanz, M., McDonald, M., Nowak, M., Phlips, B.F., Remillard, R., Stevens, A.L., Tomsick, J., Watts, A., Wood, K.S., Zane, S., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics
Abstract

We describe a probe-class mission concept that provides an unprecedented view of the X-ray sky, performing timing and 0.2-30 keV spectroscopy over timescales from microseconds to years. The Spectroscopic Time-Resolving Observatory for Broadband Energy X-rays (STROBE-X) has three key science drivers: (1) measuring the spin distribution of accreting black holes, (2) understanding the equation of state of dense matter, and (3) exploring the properties of the precursors and electromagnetic counterparts of gravitational wave sources. To perform these science investigations, STROBE-X comprises three primary instruments. The first uses an array of lightweight optics (3-m focal length) that concentrate incident photons onto solid state detectors with CCD-level (85-130 eV) energy resolution, 100 ns time resolution, and low background rates to cover the 0.2-12 keV band. This technology is scaled up from NICER, with enhanced optics to take advantage of the longer focal length of STROBE-X. The second uses large-area collimated silicon drift detectors, developed for ESA's LOFT, to cover the 2-30 keV band. These two instruments, with effective areas of 2 m2 at 1.5 keV and 5 m2 at 10 keV, respectively, each provide an order of magnitude improvement in effective area compared with its predecessor (NICER and RXTE, respectively). Finally, a sensitive sky monitor triggers pointed observations, provides high duty cycle, high time resolution, high spectral resolution monitoring of the X-ray sky with ~20 times the sensitivity of the RXTE ASM, and enables multi-wavelength and multi-messenger studies on a continuous, rather than scanning basis. The STROBE-X mission concept is a rapidly repointable observatory in low-Earth orbit, similar to RXTE or Swift, and will be presented to the 2020 Astrophysics Decadal Survey for consideration as a probe-class mission.

Published
2019

20. Radio frequency timing analysis of the compact jet in the black hole X-ray binary Cygnus X-1

Author

Tetarenko, A.J., Casella, P., Miller-Jones, James, Sivakoff, G.R., Tetarenko, B.E., Maccarone, T.J., Gandhi, P., Eikenberry, S., Tetarenko, A.J., Casella, P., Miller-Jones, James, Sivakoff, G.R., Tetarenko, B.E., Maccarone, T.J., Gandhi, P., and Eikenberry, S.

Abstract

© 2019 The Author(s). We present simultaneous multiband radio and X-ray observations of the black hole X-ray binary Cygnus X-1, taken with the Karl G. Jansky Very Large Array and the Nuclear Spectroscopic Telescope Array. With these data, we detect clear flux variability consistent with emission from a variable compact jet. To probe how the variability signal propagates down the jet flow, we perform detailed timing analyses of our data. We find that the radio jet emission shows no significant power at Fourier frequencies f 0.03 Hz (below ∼30 s time-scales), and that the higher frequency radio bands (9/11 GHz) are strongly correlated over a range of time-scales, displaying a roughly constant time lag with Fourier frequency of a few tens of seconds. However, in the lower frequency radio bands (2.5/3.5 GHz), we find a significant loss of coherence over the same range of time-scales. Further, we detect a correlation between the X-ray/radio emission, measuring time lags between the X-ray/radio bands on the order of tens of minutes. We use these lags to solve for the compact jet speed, finding that the Cyg X-1 jet is more relativistic than usually assumed for compact jets, where β = 0.92+.0.03−0.06 and ( = 2.59+0.79−0.61). Lastly, we constrain how the jet size scale changes with frequency, finding a shallower relation (∝ν−0.4) than predicted by simple jet models (∝ν−1), and estimate a jet opening angle of φ ∼ 0.4-1.8 deg. With this study we have developed observational techniques designed to overcome the challenges of radio timing analyses and created the tools needed to connect rapid radio jet variability properties to internal jet physics.

Published
2019

21. ALMA observations of A0620–00: Fresh clues on the nature of quiescent black hole X-ray binary jets

Author

Gallo, E., Teague, R., Plotkin, Richard, Miller-Jones, James, Russell, D.M., Dinçer, T., Bailyn, C., Maccarone, T.J., Markoff, S., Fender, R.P., Gallo, E., Teague, R., Plotkin, Richard, Miller-Jones, James, Russell, D.M., Dinçer, T., Bailyn, C., Maccarone, T.J., Markoff, S., and Fender, R.P.

Abstract

© 2019 The Author(s). We report on Atacama Large Millimeter Array (ALMA) continuum observations of the black hole X-ray binary A0620–00 at an X-ray luminosity nine orders of magnitude sub-Eddington. The system was significantly detected at 98 GHz (at 44 ± 7 μJy) and only marginally at 233 GHz (20 ± 8 μJy), about 40 d later. These results suggest either an optically thin sub-mm synchrotron spectrum, or highly variable sub-mm jet emission on month time-scales. Although the latter appears more likely, we note that, at the time of the ALMA observations, A0620–00 was in a somewhat less active optical-IR state than during all published multiwavelength campaigns when a flat-spectrum, partially self-absorbed jet has been suggested to extend from the radio to the mid-IR regime. Either interpretation is viable in the context of an internal shock model, where the jet’s spectral shape and variability are set by the power density spectrum of the shells’ Lorentz factor fluctuations. While strictly simultaneous radio–mm-IR observations are necessary to draw definitive conclusions for A0620–00, the data presented here, in combination with recent radio and sub-mm results from higher luminosity systems, demonstrate that jets from black hole X-ray binaries exhibit a high level of variability – either in flux density or intrinsic spectral shape, or both – across a wide spectrum of Eddington ratios. This is not in contrast with expectations from an internal shock model, where lower jet power systems can be expected to exhibit larger fractional variability owing to an overall decrease in synchrotron absorption.

Published
2019

22. Constraining the nature of the accreting binary in CXOGBS J174623.5−310550

Author

Perez Torres, M.A., Repetto, S., Wevers, T., Heida, M., Jonker, P.G., Hynes, R.I., Nelemans, G., Kostrzewa-Rutkowska, Z., Wyrzykowski, L., Britt, C.T., Heinke, C.O., Casares, J., Johnson, C.B., Maccarone, T.J., Steeghs, D.T.H., Perez Torres, M.A., Repetto, S., Wevers, T., Heida, M., Jonker, P.G., Hynes, R.I., Nelemans, G., Kostrzewa-Rutkowska, Z., Wyrzykowski, L., Britt, C.T., Heinke, C.O., Casares, J., Johnson, C.B., Maccarone, T.J., and Steeghs, D.T.H.

Abstract

Contains fulltext : 204348.pdf (publisher's version ) (Open Access)

Published
2019

23. Potential kick velocity distribution of black hole X-ray binaries and implications for natal kicks

Author

Atri, P., Miller-Jones, J.C.A., Bahramian, A., Plotkin, R.M., Jonker, P.G., Nelemans, G.A., Maccarone, T.J., Sivakoff, G.R., Deller, A.T., Chaty, S., Torres, M.A.P., Horiuchi, S., McCallum, J., Natusch, T., Phillips, C.J., Stevens, J., Weston, S., Atri, P., Miller-Jones, J.C.A., Bahramian, A., Plotkin, R.M., Jonker, P.G., Nelemans, G.A., Maccarone, T.J., Sivakoff, G.R., Deller, A.T., Chaty, S., Torres, M.A.P., Horiuchi, S., McCallum, J., Natusch, T., Phillips, C.J., Stevens, J., and Weston, S.

Abstract

Contains fulltext : 207551.pdf (publisher's version ) (Open Access)

Published
2019

24. Fast infrared photometry of the black-hole candidate MAXI J1820+070

Author

Casella, P., Vincentelli, F., O'Brien, K., Testa, V., Maccarone, T.J., Uttley, P., Fender, R., Russell, D.M., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

We report on near-infrared fast-photometry observations of the newly discovered X-ray transient MAXI J1820+070 (ATel #11399, #11400, #11406, #11418, #11420, , #11421, #11423, #11424, #11425, #11426, #11427, #11432, #11437, #11439, #11440, #11445), carried out with HAWK-I at VLT/Paranal.

Published
2018

25. A Radio Frequency Study of the Accreting Millisecond X-ray Pulsar, IGR J16597-3704, in the Globular Cluster NGC 6256

Author

Tetarenko, A.J., Bahramian, A., Wijnands, R., Heinke, C.O., Maccarone, T.J., Strader, J., Miller-Jones, J.C.A., Chomiuk, L., Degenaar, N., Sivakoff, G.R., Altamirano, D., Deller, A.T., Kennea, J.A., Li, K.L., Plotkin, R.M., Russell, T.D., Shaw, A.W., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Jansky, Neutron star, Pulsar, Space and Planetary Science, Observatory, Globular cluster, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Radio frequency, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, X-ray pulsar
Abstract

We present Karl G. Jansky Very Large Array radio frequency observations of the new accreting millisecond X-ray pulsar (AMXP), IGR J16597$-$3704, located in the globular cluster NGC 6256. With these data, we detect a radio counterpart to IGR J16597$-$3704, and determine an improved source position. Pairing our radio observations with quasi-simultaneous Swift/XRT X-ray observations, we place IGR J16597$-$3704 on the radio -- X-ray luminosity plane, where we find that IGR J16597$-$3704 is one of the more radio-quiet neutron star low-mass X-ray binaries known to date. We discuss the mechanisms that may govern radio luminosity (and in turn jet production and evolution) in AMXPs. Further, we use our derived radio position to search for a counterpart in archival Hubble Space Telescope and Chandra X-ray Observatory data, and estimate an upper limit on the X-ray luminosity of IGR J16597$-$3704 during quiescence., Comment: 12 pages, 4 Figures, Accepted to ApJ

Published
2018

26. STROBE-X: A probe-class mission for x-ray spectroscopy and timing on timescales from microseconds to years

Author

Ray, P.S., Arzoumanian, Z., Brandt, S., Burns, E., Chakrabarty, D., Feroci, M., Gendreau, K.C., Gevin, O., Hernanz, M., Jenke, P., Kenyon, S., Gálvez, J.L., Maccarone, T.J., Okajima, T., Remillard, R.A., Schanne, S., Tenzer, C., Vacchi, A., Wilson-Hodge, C.A., Winter, B., Zane, S., Ballantyne, D.R., Bozzo, E., Brenneman, L.W., Cackett, E., De Rosa, A., Goldstein, A., Hartmann, D.H., McDonald, M., Stevens, A.L., Tomsick, J.A., Watts, A.L., Wood, K.S., Zoghbi, A., den Herder, J.-W.A., Nikzad, S., Nakazawa, K., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, High Energy Astrophys. & Astropart. Phys (API, FNWI), den Herder, Jan-Willem A., Nikzad, Shouleh, and Nakazawa, Kazuhiro

Subjects
Photon, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Collimators, FOS: Physical sciences, Field of view, 01 natural sciences, 7. Clean energy, Collimated light, neutron stars, Neutron stars, X-ray, Optics, Silicon drift detectors, Observatory, 0103 physical sciences, Broadband, STROBE-X, Electronic, Focal length, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Optical and Magnetic Materials, Electrical and Electronic Engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, media_common, Physics, Black holes, 010308 nuclear & particles physics, business.industry, Applied Mathematics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, black holes, collimators, silicon drift detectors, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Sky, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We describe the Spectroscopic Time-Resolving Observatory for Broadband Energy X-rays (STROBE-X), a probe-class mission concept that will provide an unprecedented view of the X-ray sky, performing timing and spectroscopy over both a broad energy band (0.2-30 keV) and a wide range of timescales from microseconds to years. STROBE-X comprises two narrow-field instruments and a wide field monitor. The soft or low-energy band (0.2-12 keV) is covered by an array of lightweight optics (3-m focal length) that concentrate incident photons onto small solid-state detectors with CCD-level (85-175 eV) energy resolution, 100 ns time resolution, and low background rates. This technology has been fully developed for NICER and will be scaled up to take advantage of the longer focal length of STROBE-X. The higher-energy band (2-30 keV) is covered by large-area, collimated silicon drift detectors that were developed for the European LOFT mission concept. Each instrument will provide an order of magnitude improvement in effective area over its predecessor (NICER in the soft band and RXTE in the hard band). Finally, STROBE-X offers a sensitive wide-field monitor (WFM), both to act as a trigger for pointed observations of X-ray transients and also to provide high duty-cycle, high time-resolution, and high spectral-resolution monitoring of the variable X-ray sky. The WFM will boast approximately 20 times the sensitivity of the RXTE All-Sky Monitor, enabling multi-wavelength and multi-messenger investigations with a large instantaneous field of view. This mission concept will be presented to the 2020 Decadal Survey for consideration., 20 pages, 10 figures, to appear in Proc. SPIE Astronomical Telescopes and Instrumentation 2018

Published
2018

27. Chandra follow-up

Author

Maccarone, T.J., Bahramian, A., Heinke, C.O., Shaw, A., Sivakoff, G., Kennea, J., Wijnands, R., Degenaar, N., Strader, J., in't Zand, J., Kuulkers, E., Chakrabarty, D., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

We observed Swift J1752339-290952 (ATel #10422) with Chandra with ACIS-Svia a Director's Discretionary Time program. The data were taken starting on 2017-05-25 at 3:22:23 TT for ~8 ks. Eight photons were detected, indicating that the source has faded by a factor of several hundred since the original reported detection.

Published
2017

28. Radio Non-Detection of the New Swift Bulge Survey Transient, Swift J175233.9-290952

Author

Tetarenko, A.J., Sivakoff, G.R., Heinke, C.O., Shaw, A.W., Bahramian, A., Strader, J., Kennea, J.A., Maccarone, T.J., Wijnands, R., Degenaar, N., In't Zand, J.J.M., Kuulkers, E., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

We report follow-up VLA radio observations of the new X-ray transient, Swift J175233.9-290952, discovered with the Swift Bulge Survey (ATel #10355). Our VLA observations occurred on 2017 May 13, with scans on source between 10:13:06-11:12:54 UTC (MJD=57886.43-57886.47), in X band(8-12 GHz).

Published
2017

29. Variability from 1SXPS J1742150-291453: a very nearby X-ray source?

Author

Maccarone, T.J., Bahramian, A., Heinke, C., Shaw, A., Sivakoff, G., Kennea, J., Wijnands, R., Degenaar, N., Strader, J., in't Zand, J., Kuulkers, E., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

We report the discovery of likely flaring activity from 1SXPSJ1742150-291453 as part of the ongoing Swift Bulge Survey (ATel #10265). On May 19 at 14:43 the source was detected with 4 counts in 60 seconds(0.3-10 keV).

Published
2017

30. Discovery of a new X-ray transient, Swift J175233.9-290952, in the Swift Bulge Survey

Author

Bahramian, A., Heinke, C.O., Shaw, A.W., Strader, J., Kennea, J.A., Sivakoff, G.R., Wijnands, R., Maccarone, T.J., Kuulkers, E., in't Zand, J.J.M., Degenaar, N., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The Swift Bulge Survey is a wide and shallow imaging survey of 16 square degrees of the Galactic Bulge around the Galactic Center, to be performed every other week for 15 epochs (of 60 second exposures) when the Galactic Bulge is visible (ATels #10265, #10273, #10305).

Published
2017

31. NIR follow-up observations of the IGR J17445-2747 field

Author

Shaw, A.W., Heinke, C.O., Sivakoff, G.R., Bahramian, A., Strader, J., Maccarone, T.J., Kennea, J.A., Kuulkers, E., In't Zand, J. J.M., Wijnands, R., Degenaar, N., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We have recently initiated the Swift Bulge Survey, a wide and shallowSwift/XRT imaging survey of 16 square degrees of the Galactic Bulge around the Galactic Center, to be performed every other week for 15 epochs when the Galactic Bulge is visible.

Published
2017

32. Radio Non-Detection of the Currently Outbursting Transient Source in NGC 6440

Author

Tetarenko, A.J., Bahramian, A., Sivakoff, G.R., Heinke, C.O., Shaw, A.W., Wijnands, R., Degenaar, N., Chomiuk, L., Miller-Jones, J.C.A., Plotkin, R., Kuulkers, E., Strader, J., Tremou, E., Kennea, J.A., Altamirano, D., in 't Zand, J.J.M., Deller, A., Maccarone, T.J., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

We report follow-up VLA radio observations of NGC 6440, which has recently shown evidence of transient X-ray activity (ATel #10821, #10826). Our VLA observations occurred on 2017 Oct 11, with scans on source between 01:07:09 - 02:48:18 UTC (MJD = 58037.0466 - 58037.1169), in X band (8 - 12 GHz).

Published
2017

33. Spectroscopic classification of X-ray sources in the Galactic Bulge Survey

Author

Wevers, T., Torres, M.A.P., Jonker, P.G., Nelemans, G.A., Heinke, C., Mata Sánchez, D., Johnson, C.B., Gazer, R., Steeghs, D.T.H., Maccarone, T.J., Hynes, R.I., Casares, J., Udalski, A., Wetuski, J., Britt, C.T., Kostrzewa-Rutkowska, Z.P., Wyrzykowski, Ł., Wevers, T., Torres, M.A.P., Jonker, P.G., Nelemans, G.A., Heinke, C., Mata Sánchez, D., Johnson, C.B., Gazer, R., Steeghs, D.T.H., Maccarone, T.J., Hynes, R.I., Casares, J., Udalski, A., Wetuski, J., Britt, C.T., Kostrzewa-Rutkowska, Z.P., and Wyrzykowski, Ł.

Abstract

Contains fulltext : 176443.pdf (preprint version ) (Open Access)

Published
2017

35. Swift observation of GRS 1736-297

Author

Bahramian, A., Heinke, C.O., Sivakoff, G.R., Maccarone, T.J., Wijnands, R., Degenaar, N., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

GRS 1736-297 is an X-ray transient near the Galactic center. The source was last detected in outburst in 2006 (ATel #744). Recently, INTEGRAL detected a new outburst of the source (ATel #8698).

Published
2016

37. Candidate Hα emission and absorption line sources in the Galactic Bulge Survey

Author

Wevers, T., Jonker, P.G., Nelemans, G.A., Torres, M.A.P., Groot, P.J., Steeghs, D., Maccarone, T.J., Hynes, R.I., Heinke, C., Britt, C., Wevers, T., Jonker, P.G., Nelemans, G.A., Torres, M.A.P., Groot, P.J., Steeghs, D., Maccarone, T.J., Hynes, R.I., Heinke, C., and Britt, C.

Abstract

Contains fulltext : 163264.pdf (publisher's version ) (Open Access)

Published
2016

38. The peculiar dipping events in the disk-bearing young-stellar object EPIC 204278916

Author

Scaringi, S., Manara, C.F., Barenfeld, S.A., Groot, P.J., Isella, A., Kenworthy, M.A., Knigge, C., Maccarone, T.J., Ricci, L., Ansdell, M., Scaringi, S., Manara, C.F., Barenfeld, S.A., Groot, P.J., Isella, A., Kenworthy, M.A., Knigge, C., Maccarone, T.J., Ricci, L., and Ansdell, M.

Abstract

Contains fulltext : 161672.pdf (preprint version ) (Open Access)

Published
2016

39. Discovery of a high state AM CVn binary in the Galactic Bulge Survey

Author

Wevers, T., Torres, M.A.P., Jonker, P.G., Wetuski, J.D., Nelemans, G.A., Steeghs, D., Maccarone, T.J., Heinke, C., Hynes, R.I., Udalski, A., Kostrzewa-Rutkowska, Z.P., Groot, P.J., Gazer, R., Szymański, M.K., Britt, C.T., Wyrzykowski, Ł., Poleski, R., Wevers, T., Torres, M.A.P., Jonker, P.G., Wetuski, J.D., Nelemans, G.A., Steeghs, D., Maccarone, T.J., Heinke, C., Hynes, R.I., Udalski, A., Kostrzewa-Rutkowska, Z.P., Groot, P.J., Gazer, R., Szymański, M.K., Britt, C.T., Wyrzykowski, Ł., and Poleski, R.

Abstract

Contains fulltext : 159643.pdf (preprint version ) (Open Access)

Published
2016

40. The First Low-mass Black Hole X-Ray Binary Identified in Quiescence Outside of a Globular Cluster

Author

Tetarenko, B.E., Bahramian, A., Arnason, R.M., Miller-Jones, J.C.A., Repetto, S., Heinke, C.O., Maccarone, T.J., Chomiuk, L., Sivakoff, G.R., Strader, J., Kirsten, F., Vlemmings, W., Tetarenko, B.E., Bahramian, A., Arnason, R.M., Miller-Jones, J.C.A., Repetto, S., Heinke, C.O., Maccarone, T.J., Chomiuk, L., Sivakoff, G.R., Strader, J., Kirsten, F., and Vlemmings, W.

Abstract

Contains fulltext : 159677.pdf (publisher's version ) (Open Access)

Published
2016

41. Discovery of a long-lived, high-amplitude dusty infrared transient

Author

Britt, C.T., Maccarone, T.J., Green, J.D., Jonker, P.G., Hynes, R.I., Torres, M.A.P., Strader, J., Chomiuk, L., Salinas, R., Lucas, P, Contreras Peña, C., Kurtev, R., Heinke, C., Smith, L., Wright, N.J., Johnson, C., Steeghs, D., Nelemans, G.A., Britt, C.T., Maccarone, T.J., Green, J.D., Jonker, P.G., Hynes, R.I., Torres, M.A.P., Strader, J., Chomiuk, L., Salinas, R., Lucas, P, Contreras Peña, C., Kurtev, R., Heinke, C., Smith, L., Wright, N.J., Johnson, C., Steeghs, D., and Nelemans, G.A.

Abstract

Contains fulltext : 159644.pdf (preprint version ) (Open Access), We report the detection of an infrared-selected transient which has lasted at least five years, first identified by a large mid-infrared and optical outburst from a faint X-ray source detected with the Chandra X-ray Observatory. In this paper we rule out several scenarios for the cause of this outburst, including a classical nova, a luminous red nova, AGN flaring, a stellar merger, and intermediate luminosity optical transients, and interpret this transient as the result of a young stellar object (YSO) of at least solar mass accreting material from the remains of the dusty envelope from which it formed, in isolation from either a dense complex of cold gas or massive star formation. This object does not fit neatly into other existing categories of large outbursts of YSOs (FU Orionis types) which may be a result of the object's mass, age, and environment. It is also possible that this object is a new type of transient unrelated to YSOs.

Published
2016

42. The Chandra Galactic Bulge Survey: optical catalogue and point-source counterparts to X-ray sources

Author

Wevers, T., Hodgkin, S.T., Jonker, P.G., Bassa, C., Nelemans, G.A., Grunsven, T. van, Gonzalez-Solares, E.A., Torres, M.A.P., Heinke, C., Steeghs, D., Maccarone, T.J., Britt, C., Hynes, R.I., Johnson, C., Wu, J., Wevers, T., Hodgkin, S.T., Jonker, P.G., Bassa, C., Nelemans, G.A., Grunsven, T. van, Gonzalez-Solares, E.A., Torres, M.A.P., Heinke, C., Steeghs, D., Maccarone, T.J., Britt, C., Hynes, R.I., Johnson, C., and Wu, J.

Abstract

Contains fulltext : 157954.pdf (publisher's version ) (Open Access)

Published
2016

46. Gemini spectroscopy of Galactic Bulge Sources: a population of hidden accreting binaries revealed?

Author

Wu, J., Jonker, P.G., Torres, M.A.P., Britt, C.T., Johnson, C.B., Hynes, R.I., Greiss, S., Steeghs, D.T.H., Maccarone, T.J., Heinke, C.O., Wevers, T., Wu, J., Jonker, P.G., Torres, M.A.P., Britt, C.T., Johnson, C.B., Hynes, R.I., Greiss, S., Steeghs, D.T.H., Maccarone, T.J., Heinke, C.O., and Wevers, T.

Abstract

Contains fulltext : 141154.pdf (preprint version ) (Open Access)

Published
2015

49. X-ray softening in the new X-ray transient XTE J1719-291 during its 2008 outburst decay

Author

Armas Padilla, M., Degenaar, N., Patruno, A., Russell, D.M., Linares, M., Maccarone, T.J., Homan, J., Wijnands, R., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

The X-ray transient XTE J1719-291 was discovered with RXTE/PCA during its outburst in 2008 March, which lasted at least 46 days. Its 2-10 keV peak luminosity is 7E35 erg/s assuming a distance of 8 kpc, which classifies the system as a very faint X-ray transient. The outburst was monitored with Swift, RXTE, Chandra and XMM-Newton. We analysed the X-ray spectral evolution during the outburst. We fitted the overall data with a simple power-law model corrected for absorption and found that the spectrum softened with decreasing luminosity. However, the XMM-Newton spectrum can not be fitted with a simple one-component model, but it can be fitted with a thermal component (black body or disc black body) plus power-law model affected by absorption. Therefore, the softening of the X-ray spectrum with decreasing X-ray luminosity might be due to a change in photon index or alternatively it might be due to a change in the properties of the soft component. Assuming that the system is an X-ray binary, we estimated a long-term time-averaged mass accretion rate of ~ 7.7E-13 M_sun/yr for a neutron star as compact object and ~ 3.7E10-13 M_sun/yr in the case of a black hole. Although no conclusive evidence is available about the nature of the accretor, based on the X-ray/optical luminosity ratio we tentatively suggest that a neutron star is present in this system., Accepted for publication in MNRAS. 8 pages, 4 figures, 2 tables

Published
2011
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50. Coupling between QPOs and broad-band noise components in GRS 1915+105

Author

Maccarone, T.J., Uttley, P., van der Klis, M., Wijnands, R.A.D., Coppi, P.S., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

We explore the use of the bispectrum for understanding quasi-periodic oscillations. The bispectrum is a statistic which probes the relations between the relative phases of the Fourier spectrum at different frequencies. The use of the bispectrum allows us to break the degeneracies between different models for time series which produce identical power spectra. We look at data from several observations of GRS 1915+105 when the source shows strong quasi-periodic oscillations and strong broad-band noise components in its power spectrum. We show that, despite strong similarities in the power spectrum, the bispectra can differ strongly. In all cases, there are frequency ranges where the bicoherence, a measure of non-linearity, is strong for frequencies involving the frequency of the quasi-periodic oscillations, indicating that the quasi-periodic oscillations are coupled to the noise components, rather than being generated independently. We compare the bicoherences from the data to simple models, finding some qualitative similarities.

Published
2011

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