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1. Euclid. III. The NISP Instrument

Author

Euclid Collaboration, Jahnke, K., Gillard, W., Schirmer, M., Ealet, A., Maciaszek, T., Prieto, E., Barbier, R., Bonoli, C., Corcione, L., Dusini, S., Grupp, F., Hormuth, F., Ligori, S., Martin, L., Morgante, G., Padilla, C., Toledo-Moreo, R., Trifoglio, M., Valenziano, L., Bender, R., Castander, F. J., Garilli, B., Lilje, P. B., Rix, H. -W., Auricchio, N., Balestra, A., Barriere, J. -C., Battaglia, P., Berthe, M., Bodendorf, C., Boenke, T., Bon, W., Bonnefoi, A., Caillat, A., Capobianco, V., Carle, M., Casas, R., Cho, H., Costille, A., Ducret, F., Ferriol, S., Franceschi, E., Gimenez, J. -L., Holmes, W., Hornstrup, A., Jhabvala, M., Kohley, R., Kubik, B., Laureijs, R., Mignant, D. Le, Lloro, I., Medinaceli, E., Mellier, Y., Polenta, G., Racca, G. D., Renzi, A., Salvignol, J. -C., Secroun, A., Seidel, G., Seiffert, M., Sirignano, C., Sirri, G., Strada, P., Smadja, G., Stanco, L., Wachter, S., Anselmi, S., Borsato, E., Caillat, L., Cogato, F., Colodro-Conde, C., Crouzet, P. -E., Conforti, V., D'Alessandro, M., Copin, Y., Cuillandre, J. -C., Davies, J. E., Davini, S., Derosa, A., Diaz, J. J., Di Domizio, S., Di Ferdinando, D., Farinelli, R., Ferrari, A. G., Fornari, F., Gabarra, L., Gutierrez, C. M., Giacomini, F., Lagier, P., Gianotti, F., Krause, O., Madrid, F., Laudisio, F., Macias-Perez, J., Naletto, G., Niclas, M., Marpaud, J., Mauri, N., da Silva, R., Passalacqua, F., Paterson, K., Patrizii, L., Risso, I., Solheim, B. G. B., Scodeggio, M., Stassi, P., Steinwagner, J., Tenti, M., Testera, G., Travaglini, R., Tosi, S., Troja, A., Tubio, O., Valieri, C., Vescovi, C., Ventura, S., Aghanim, N., Altieri, B., Amara, A., Amiaux, J., Andreon, S., Aussel, H., Baldi, M., Bardelli, S., Basset, A., Bonchi, A., Bonino, D., Branchini, E., Brescia, M., Brinchmann, J., Camera, S., Carbone, C., Cardone, V. F., Carretero, J., Casas, S., Castellano, M., Cavuoti, S., Chabaud, P. -Y., Cimatti, A., Congedo, G., Conselice, C. J., Conversi, L., Courbin, F., Courtois, H. M., Cropper, M., Cuby, J. -G., Da Silva, A., Degaudenzi, H., Di Giorgio, A. M., Dinis, J., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Fabricius, M., Farina, M., Farrens, S., Faustini, F., Fosalba, P., Fotopoulou, S., Fourmanoit, N., Frailis, M., Franzetti, P., Galeotta, S., Gillis, B., Giocoli, C., Gómez-Alvarez, P., Granett, B. R., Grazian, A., Guzzo, L., Hailey, M., Haugan, S. V. H., Hoar, J., Hoekstra, H., Hook, I., Hudelot, P., Joachimi, B., Keihänen, E., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kümmel, M., Kunz, M., Kurki-Suonio, H., Lahav, O., Lindholm, V., Alvarez, J. Lorenzo, Maino, D., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Martignac, J., Martinet, N., Marulli, F., Massey, R., Masters, D. C., Maurogordato, S., McCracken, H. J., Mei, S., Melchior, M., Meneghetti, M., Merlin, E., Meylan, G., Mohr, J. J., Moresco, M., Moscardini, L., Nakajima, R., Nichol, R. C., Niemi, S. -M., Nutma, T., Paech, K., Paltani, S., Pasian, F., Peacock, J. A., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Poncet, M., Popa, L. A., Pozzetti, L., Raison, F., Rebolo, R., Refregier, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rosset, C., Rossetti, E., Rottgering, H. J. A., Saglia, R., Sapone, D., Sauvage, M., Scaramella, R., Schneider, P., Schrabback, T., Serrano, S., Tallada-Crespí, P., Tavagnacco, D., Taylor, A. N., Teplitz, H. I., Tereno, I., Torradeflot, F., Tutusaus, I., Vassallo, T., Kleijn, G. Verdoes, Veropalumbo, A., Vibert, D., Wang, Y., Weller, J., Zacchei, A., Zamorani, G., Zerbi, F. M., Zoubian, J., Zucca, E., Appleton, P. N., Baccigalupi, C., Biviano, A., Bolzonella, M., Boucaud, A., Bozzo, E., Burigana, C., Calabrese, M., Casenove, P., Crocce, M., De Lucia, G., Vigo, J. A. Escartin, Fabbian, G., Finelli, F., George, K., Gracia-Carpio, J., Ilić, S., Liebing, P., Liu, C., Mainetti, G., Marcin, S., Martinelli, M., Morris, P. W., Neissner, C., Pezzotta, A., Pöntinen, M., Porciani, C., Sakr, Z., Scottez, V., Sefusatti, E., Viel, M., Wiesmann, M., Akrami, Y., Allevato, V., Aubourg, E., Ballardini, M., Bertacca, D., Bethermin, M., Blanchard, A., Blot, L., Borgani, S., Borlaff, A. S., Bruton, S., Cabanac, R., Calabro, A., Calderone, G., Canas-Herrera, G., Cappi, A., Carvalho, C. S., Castignani, G., Castro, T., Chambers, K. C., Charles, Y., Chary, R., Colbert, J., Contarini, S., Contini, T., Cooray, A. R., Costanzi, M., Cucciati, O., De Caro, B., de la Torre, S., Desprez, G., Díaz-Sánchez, A., Dole, H., Escoffier, S., Ferreira, P. G., Ferrero, I., Finoguenov, A., Fontana, A., Ganga, K., García-Bellido, J., Gautard, V., Gaztanaga, E., Gozaliasl, G., Gregorio, A., Hall, A., Hartley, W. G., Hemmati, S., Hildebrandt, H., Hjorth, J., Hosseini, S., Huertas-Company, M., Ilbert, O., Jacobson, J., Joudaki, S., Kajava, J. J. E., Kansal, V., Karagiannis, D., Kirkpatrick, C. C., Lacasa, F., Brun, V. Le, Graet, J. Le, Legrand, L., Libet, G., Liu, S. J., Loureiro, A., Magliocchetti, M., Mancini, C., Mannucci, F., Maoli, R., Martins, C. J. A. P., Matthew, S., Maurin, L., McPartland, C. J. R., Metcalf, R. B., Migliaccio, M., Miluzio, M., Monaco, P., Moretti, C., Nadathur, S., Nicastro, L., Walton, Nicholas A., Odier, J., Oguri, M., Popa, V., Potter, D., Pourtsidou, A., Rocci, P. -F., Rollins, R. P., Rusholme, B., Sahlén, M., Sánchez, A. G., Scarlata, C., Schaye, J., Schewtschenko, J. A., Schneider, A., Schultheis, M., Sereno, M., Shankar, F., Shulevski, A., Sikkema, G., Silvestri, A., Simon, P., Mancini, A. Spurio, Stadel, J., Stanford, S. A., Tanidis, K., Tao, C., Tessore, N., Teyssier, R., Toft, S., Tucci, M., Valiviita, J., Vergani, D., Vernizzi, F., Verza, G., Vielzeuf, P., Weaver, J. R., Zalesky, L., Zinchenko, I. A., Archidiacono, M., Atrio-Barandela, F., Bennett, C. L., Bouvard, T., Caro, F., Conseil, S., Dimauro, P., Duc, P. -A., Fang, Y., Ferguson, A. M. N., Gasparetto, T., Kova{č}ić, I., Kruk, S., Brun, A. M. C. Le, Liaudat, T. I., Montoro, A., Mora, A., Murray, C., Pagano, L., Paoletti, D., Radovich, M., Sarpa, E., Tommasi, E., Viitanen, A., Lesgourgues, J., Levi, M. E., and Martín-Fleitas, J.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The Near-Infrared Spectrometer and Photometer (NISP) on board the Euclid satellite provides multiband photometry and R>=450 slitless grism spectroscopy in the 950-2020nm wavelength range. In this reference article we illuminate the background of NISP's functional and calibration requirements, describe the instrument's integral components, and provide all its key properties. We also sketch the processes needed to understand how NISP operates and is calibrated, and its technical potentials and limitations. Links to articles providing more details and technical background are included. NISP's 16 HAWAII-2RG (H2RG) detectors with a plate scale of 0.3" pix^-1 deliver a field-of-view of 0.57deg^2. In photo mode, NISP reaches a limiting magnitude of ~24.5AB mag in three photometric exposures of about 100s exposure time, for point sources and with a signal-to-noise ratio (SNR) of 5. For spectroscopy, NISP's point-source sensitivity is a SNR = 3.5 detection of an emission line with flux ~2x10^-16erg/s/cm^2 integrated over two resolution elements of 13.4A, in 3x560s grism exposures at 1.6 mu (redshifted Ha). Our calibration includes on-ground and in-flight characterisation and monitoring of detector baseline, dark current, non-linearity, and sensitivity, to guarantee a relative photometric accuracy of better than 1.5%, and relative spectrophotometry to better than 0.7%. The wavelength calibration must be better than 5A. NISP is the state-of-the-art instrument in the NIR for all science beyond small areas available from HST and JWST - and an enormous advance due to its combination of field size and high throughput of telescope and instrument. During Euclid's 6-year survey covering 14000 deg^2 of extragalactic sky, NISP will be the backbone for determining distances of more than a billion galaxies. Its NIR data will become a rich reference imaging and spectroscopy data set for the coming decades., Comment: Paper submitted as part of the A&A special issue 'Euclid on Sky', which contains Euclid key reference papers and first results from the Euclid Early Release Observations

Published
2024

2. Euclid. I. Overview of the Euclid mission

Author

Euclid Collaboration, Mellier, Y., Abdurro'uf, Barroso, J. A. Acevedo, Achúcarro, A., Adamek, J., Adam, R., Addison, G. E., Aghanim, N., Aguena, M., Ajani, V., Akrami, Y., Al-Bahlawan, A., Alavi, A., Albuquerque, I. S., Alestas, G., Alguero, G., Allaoui, A., Allen, S. W., Allevato, V., Alonso-Tetilla, A. V., Altieri, B., Alvarez-Candal, A., Alvi, S., Amara, A., Amendola, L., Amiaux, J., Andika, I. T., Andreon, S., Andrews, A., Angora, G., Angulo, R. E., Annibali, F., Anselmi, A., Anselmi, S., Arcari, S., Archidiacono, M., Aricò, G., Arnaud, M., Arnouts, S., Asgari, M., Asorey, J., Atayde, L., Atek, H., Atrio-Barandela, F., Aubert, M., Aubourg, E., Auphan, T., Auricchio, N., Aussel, B., Aussel, H., Avelino, P. P., Avgoustidis, A., Avila, S., Awan, S., Azzollini, R., Baccigalupi, C., Bachelet, E., Bacon, D., Baes, M., Bagley, M. B., Bahr-Kalus, B., Balaguera-Antolinez, A., Balbinot, E., Balcells, M., Baldi, M., Baldry, I., Balestra, A., Ballardini, M., Ballester, O., Balogh, M., Bañados, E., Barbier, R., Bardelli, S., Baron, M., Barreiro, T., Barrena, R., Barriere, J. -C., Barros, B. J., Barthelemy, A., Bartolo, N., Basset, A., Battaglia, P., Battisti, A. J., Baugh, C. M., Baumont, L., Bazzanini, L., Beaulieu, J. -P., Beckmann, V., Belikov, A. N., Bel, J., Bellagamba, F., Bella, M., Bellini, E., Benabed, K., Bender, R., Benevento, G., Bennett, C. L., Benson, K., Bergamini, P., Bermejo-Climent, J. R., Bernardeau, F., Bertacca, D., Berthe, M., Berthier, J., Bethermin, M., Beutler, F., Bevillon, C., Bhargava, S., Bhatawdekar, R., Bianchi, D., Bisigello, L., Biviano, A., Blake, R. P., Blanchard, A., Blazek, J., Blot, L., Bosco, A., Bodendorf, C., Boenke, T., Böhringer, H., Boldrini, P., Bolzonella, M., Bonchi, A., Bonici, M., Bonino, D., Bonino, L., Bonvin, C., Bon, W., Booth, J. T., Borgani, S., Borlaff, A. S., Borsato, E., Bose, B., Botticella, M. T., Boucaud, A., Bouche, F., Boucher, J. S., Boutigny, D., Bouvard, T., Bouwens, R., Bouy, H., Bowler, R. A. A., Bozza, V., Bozzo, E., Branchini, E., Brando, G., Brau-Nogue, S., Brekke, P., Bremer, M. N., Brescia, M., Breton, M. -A., Brinchmann, J., Brinckmann, T., Brockley-Blatt, C., Brodwin, M., Brouard, L., Brown, M. L., Bruton, S., Bucko, J., Buddelmeijer, H., Buenadicha, G., Buitrago, F., Burger, P., Burigana, C., Busillo, V., Busonero, D., Cabanac, R., Cabayol-Garcia, L., Cagliari, M. S., Caillat, A., Caillat, L., Calabrese, M., Calabro, A., Calderone, G., Calura, F., Quevedo, B. Camacho, Camera, S., Campos, L., Canas-Herrera, G., Candini, G. P., Cantiello, M., Capobianco, V., Cappellaro, E., Cappelluti, N., Cappi, A., Caputi, K. I., Cara, C., Carbone, C., Cardone, V. F., Carella, E., Carlberg, R. G., Carle, M., Carminati, L., Caro, F., Carrasco, J. M., Carretero, J., Carrilho, P., Duque, J. Carron, Carry, B., Carvalho, A., Carvalho, C. S., Casas, R., Casas, S., Casenove, P., Casey, C. M., Cassata, P., Castander, F. J., Castelao, D., Castellano, M., Castiblanco, L., Castignani, G., Castro, T., Cavet, C., Cavuoti, S., Chabaud, P. -Y., Chambers, K. C., Charles, Y., Charlot, S., Chartab, N., Chary, R., Chaumeil, F., Cho, H., Chon, G., Ciancetta, E., Ciliegi, P., Cimatti, A., Cimino, M., Cioni, M. -R. L., Claydon, R., Cleland, C., Clément, B., Clements, D. L., Clerc, N., Clesse, S., Codis, S., Cogato, F., Colbert, J., Cole, R. E., Coles, P., Collett, T. E., Collins, R. S., Colodro-Conde, C., Colombo, C., Combes, F., Conforti, V., Congedo, G., Conseil, S., Conselice, C. J., Contarini, S., Contini, T., Conversi, L., Cooray, A. R., Copin, Y., Corasaniti, P. -S., Corcho-Caballero, P., Corcione, L., Cordes, O., Corpace, O., Correnti, M., Costanzi, M., Costille, A., Courbin, F., Mifsud, L. Courcoult, Courtois, H. M., Cousinou, M. -C., Covone, G., Cowell, T., Cragg, C., Cresci, G., Cristiani, S., Crocce, M., Cropper, M., Crouzet, P. E, Csizi, B., Cuby, J. -G., Cucchetti, E., Cucciati, O., Cuillandre, J. -C., Cunha, P. A. C., Cuozzo, V., Daddi, E., D'Addona, M., Dafonte, C., Dagoneau, N., Dalessandro, E., Dalton, G. B., D'Amico, G., Dannerbauer, H., Danto, P., Das, I., Da Silva, A., da Silva, R., Doumerg, W. d'Assignies, Daste, G., Davies, J. E., Davini, S., Dayal, P., de Boer, T., Decarli, R., De Caro, B., Degaudenzi, H., Degni, G., de Jong, J. T. A., de la Bella, L. F., de la Torre, S., Delhaise, F., Delley, D., Delucchi, G., De Lucia, G., Denniston, J., De Paolis, F., De Petris, M., Derosa, A., Desai, S., Desjacques, V., Despali, G., Desprez, G., De Vicente-Albendea, J., Deville, Y., Dias, J. D. F., Díaz-Sánchez, A., Diaz, J. J., Di Domizio, S., Diego, J. M., Di Ferdinando, D., Di Giorgio, A. M., Dimauro, P., Dinis, J., Dolag, K., Dolding, C., Dole, H., Sánchez, H. Domínguez, Doré, O., Dournac, F., Douspis, M., Dreihahn, H., Droge, B., Dryer, B., Dubath, F., Duc, P. -A., Ducret, F., Duffy, C., Dufresne, F., Duncan, C. A. J., Dupac, X., Duret, V., Durrer, R., Durret, F., Dusini, S., Ealet, A., Eggemeier, A., Eisenhardt, P. R. M., Elbaz, D., Elkhashab, M. Y., Ellien, A., Endicott, J., Enia, A., Erben, T., Vigo, J. A. Escartin, Escoffier, S., Sanz, I. Escudero, Essert, J., Ettori, S., Ezziati, M., Fabbian, G., Fabricius, M., Fang, Y., Farina, A., Farina, M., Farinelli, R., Farrens, S., Faustini, F., Feltre, A., Ferguson, A. M. N., Ferrando, P., Ferrari, A. G., Ferré-Mateu, A., Ferreira, P. G., Ferreras, I., Ferrero, I., Ferriol, S., Ferruit, P., Filleul, D., Finelli, F., Finkelstein, S. L., Finoguenov, A., Fiorini, B., Flentge, F., Focardi, P., Fonseca, J., Fontana, A., Fontanot, F., Fornari, F., Fosalba, P., Fossati, M., Fotopoulou, S., Fouchez, D., Fourmanoit, N., Frailis, M., Fraix-Burnet, D., Franceschi, E., Franco, A., Franzetti, P., Freihoefer, J., Frenk, C. . S., Frittoli, G., Frugier, P. -A., Frusciante, N., Fumagalli, A., Fumagalli, M., Fumana, M., Fu, Y., Gabarra, L., Galeotta, S., Galluccio, L., Ganga, K., Gao, H., García-Bellido, J., Garcia, K., Gardner, J. P., Garilli, B., Gaspar-Venancio, L. -M., Gasparetto, T., Gautard, V., Gavazzi, R., Gaztanaga, E., Genolet, L., Santos, R. Genova, Gentile, F., George, K., Gerbino, M., Ghaffari, Z., Giacomini, F., Gianotti, F., Gibb, G. P. S., Gillard, W., Gillis, B., Ginolfi, M., Giocoli, C., Girardi, M., Giri, S. K., Goh, L. W. K., Gómez-Alvarez, P., Gonzalez-Perez, V., Gonzalez, A. H., Gonzalez, E. J., Gonzalez, J. C., Beauchamps, S. Gouyou, Gozaliasl, G., Gracia-Carpio, J., Grandis, S., Granett, B. R., Granvik, M., Grazian, A., Gregorio, A., Grenet, C., Grillo, C., Grupp, F., Gruppioni, C., Gruppuso, A., Guerbuez, C., Guerrini, S., Guidi, M., Guillard, P., Gutierrez, C. M., Guttridge, P., Guzzo, L., Gwyn, S., Haapala, J., Haase, J., Haddow, C. R., Hailey, M., Hall, A., Hall, D., Hamaus, N., Haridasu, B. S., Harnois-Déraps, J., Harper, C., Hartley, W. G., Hasinger, G., Hassani, F., Hatch, N. A., Haugan, S. V. H., Häußler, B., Heavens, A., Heisenberg, L., Helmi, A., Helou, G., Hemmati, S., Henares, K., Herent, O., Hernández-Monteagudo, C., Heuberger, T., Hewett, P. C., Heydenreich, S., Hildebrandt, H., Hirschmann, M., Hjorth, J., Hoar, J., Hoekstra, H., Holland, A. D., Holliman, M. S., Holmes, W., Hook, I., Horeau, B., Hormuth, F., Hornstrup, A., Hosseini, S., Hu, D., Hudelot, P., Hudson, M. J., Huertas-Company, M., Huff, E. M., Hughes, A. C. N., Humphrey, A., Hunt, L. K., Huynh, D. D., Ibata, R., Ichikawa, K., Iglesias-Groth, S., Ilbert, O., Ilić, S., Ingoglia, L., Iodice, E., Israel, H., Israelsson, U. E., Izzo, L., Jablonka, P., Jackson, N., Jacobson, J., Jafariyazani, M., Jahnke, K., Jain, B., Jansen, H., Jarvis, M. J., Jasche, J., Jauzac, M., Jeffrey, N., Jhabvala, M., Jimenez-Teja, Y., Muñoz, A. Jimenez, Joachimi, B., Johansson, P. H., Joudaki, S., Jullo, E., Kajava, J. J. E., Kang, Y., Kannawadi, A., Kansal, V., Karagiannis, D., Kärcher, M., Kashlinsky, A., Kazandjian, M. V., Keck, F., Keihänen, E., Kerins, E., Kermiche, S., Khalil, A., Kiessling, A., Kiiveri, K., Kilbinger, M., Kim, J., King, R., Kirkpatrick, C. C., Kitching, T., Kluge, M., Knabenhans, M., Knapen, J. H., Knebe, A., Kneib, J. -P., Kohley, R., Koopmans, L. V. E., Koskinen, H., Koulouridis, E., Kou, R., Kovács, A., Kovačić, I., Kowalczyk, A., Koyama, K., Kraljic, K., Krause, O., Kruk, S., Kubik, B., Kuchner, U., Kuijken, K., Kümmel, M., Kunz, M., Kurki-Suonio, H., Lacasa, F., Lacey, C. G., La Franca, F., Lagarde, N., Lahav, O., Laigle, C., La Marca, A., La Marle, O., Lamine, B., Lam, M. C., Lançon, A., Landt, H., Langer, M., Lapi, A., Larcheveque, C., Larsen, S. S., Lattanzi, M., Laudisio, F., Laugier, D., Laureijs, R., Laurent, V., Lavaux, G., Lawrenson, A., Lazanu, A., Lazeyras, T., Boulc'h, Q. Le, Brun, A. M. C. Le, Brun, V. Le, Leclercq, F., Lee, S., Graet, J. Le, Legrand, L., Leirvik, K. N., Jeune, M. Le, Lembo, M., Mignant, D. Le, Lepinzan, M. D., Lepori, F., Reun, A. Le, Leroy, G., Lesci, G. F., Lesgourgues, J., Leuzzi, L., Levi, M. E., Liaudat, T. I., Libet, G., Liebing, P., Ligori, S., Lilje, P. B., Lin, C. -C., Linde, D., Linder, E., Lindholm, V., Linke, L., Li, S. -S., Liu, S. J., Lloro, I., Lobo, F. S. N., Lodieu, N., Lombardi, M., Lombriser, L., Lonare, P., Longo, G., López-Caniego, M., Lopez, X. Lopez, Alvarez, J. Lorenzo, Loureiro, A., Loveday, J., Lusso, E., Macias-Perez, J., Maciaszek, T., Maggio, G., Magliocchetti, M., Magnard, F., Magnier, E. A., Magro, A., Mahler, G., Mainetti, G., Maino, D., Maiorano, E., Malavasi, N., Mamon, G. A., Mancini, C., Mandelbaum, R., Manera, M., Manjón-García, A., Mannucci, F., Mansutti, O., Outeiro, M. Manteiga, Maoli, R., Maraston, C., Marcin, S., Marcos-Arenal, P., Margalef-Bentabol, B., Marggraf, O., Marinucci, D., Marinucci, M., Markovic, K., Marleau, F. R., Marpaud, J., Martignac, J., Martín-Fleitas, J., Martin-Moruno, P., Martin, E. L., Martinelli, M., Martinet, N., Martin, H., Martins, C. J. A. P., Marulli, F., Massari, D., Massey, R., Masters, D. C., Matarrese, S., Matsuoka, Y., Matthew, S., Maughan, B. J., Mauri, N., Maurin, L., Maurogordato, S., McCarthy, K., McConnachie, A. W., McCracken, H. J., McDonald, I., McEwen, J. D., McPartland, C. J. R., Medinaceli, E., Mehta, V., Mei, S., Melchior, M., Melin, J. -B., Ménard, B., Mendes, J., Mendez-Abreu, J., Meneghetti, M., Mercurio, A., Merlin, E., Metcalf, R. B., Meylan, G., Migliaccio, M., Mignoli, M., Miller, L., Miluzio, M., Milvang-Jensen, B., Mimoso, J. P., Miquel, R., Miyatake, H., Mobasher, B., Mohr, J. J., Monaco, P., Monguió, M., Montoro, A., Mora, A., Dizgah, A. Moradinezhad, Moresco, M., Moretti, C., Morgante, G., Morisset, N., Moriya, T. J., Morris, P. W., Mortlock, D. J., Moscardini, L., Mota, D. F., Mottet, S., Moustakas, L. A., Moutard, T., Müller, T., Munari, E., Murphree, G., Murray, C., Murray, N., Musi, P., Nadathur, S., Nagam, B. C., Nagao, T., Naidoo, K., Nakajima, R., Nally, C., Natoli, P., Navarro-Alsina, A., Girones, D. Navarro, Neissner, C., Nersesian, A., Nesseris, S., Nguyen-Kim, H. N., Nicastro, L., Nichol, R. C., Nielbock, M., Niemi, S. -M., Nieto, S., Nilsson, K., Noller, J., Norberg, P., Nouri-Zonoz, A., Ntelis, P., Nucita, A. A., Nugent, P., Nunes, N. J., Nutma, T., Ocampo, I., Odier, J., Oesch, P. A., Oguri, M., Oliveira, D. Magalhaes, Onoue, M., Oosterbroek, T., Oppizzi, F., Ordenovic, C., Osato, K., Pacaud, F., Pace, F., Padilla, C., Paech, K., Pagano, L., Page, M. J., Palazzi, E., Paltani, S., Pamuk, S., Pandolfi, S., Paoletti, D., Paolillo, M., Papaderos, P., Pardede, K., Parimbelli, G., Parmar, A., Partmann, C., Pasian, F., Passalacqua, F., Paterson, K., Patrizii, L., Pattison, C., Paulino-Afonso, A., Paviot, R., Peacock, J. A., Pearce, F. R., Pedersen, K., Peel, A., Peletier, R. F., Ibanez, M. Pellejero, Pello, R., Penny, M. T., Percival, W. J., Perez-Garrido, A., Perotto, L., Pettorino, V., Pezzotta, A., Pezzuto, S., Philippon, A., Pierre, M., Piersanti, O., Pietroni, M., Piga, L., Pilo, L., Pires, S., Pisani, A., Pizzella, A., Pizzuti, L., Plana, C., Polenta, G., Pollack, J. E., Poncet, M., Pöntinen, M., Pool, P., Popa, L. A., Popa, V., Popp, J., Porciani, C., Porth, L., Potter, D., Poulain, M., Pourtsidou, A., Pozzetti, L., Prandoni, I., Pratt, G. W., Prezelus, S., Prieto, E., Pugno, A., Quai, S., Quilley, L., Racca, G. D., Raccanelli, A., Rácz, G., Radinović, S., Radovich, M., Ragagnin, A., Ragnit, U., Raison, F., Ramos-Chernenko, N., Ranc, C., Rasera, Y., Raylet, N., Rebolo, R., Refregier, A., Reimberg, P., Reiprich, T. H., Renk, F., Renzi, A., Retre, J., Revaz, Y., Reylé, C., Reynolds, L., Rhodes, J., Ricci, F., Ricci, M., Riccio, G., Ricken, S. O., Rissanen, S., Risso, I., Rix, H. -W., Robin, A. C., Rocca-Volmerange, B., Rocci, P. -F., Rodenhuis, M., Rodighiero, G., Monroy, M. Rodriguez, Rollins, R. P., Romanello, M., Roman, J., Romelli, E., Romero-Gomez, M., Roncarelli, M., Rosati, P., Rosset, C., Rossetti, E., Roster, W., Rottgering, H. J. A., Rozas-Fernández, A., Ruane, K., Rubino-Martin, J. A., Rudolph, A., Ruppin, F., Rusholme, B., Sacquegna, S., Sáez-Casares, I., Saga, S., Saglia, R., Sahlén, M., Saifollahi, T., Sakr, Z., Salvalaggio, J., Salvaterra, R., Salvati, L., Salvato, M., Salvignol, J. -C., Sánchez, A. G., Sanchez, E., Sanders, D. B., Sapone, D., Saponara, M., Sarpa, E., Sarron, F., Sartori, S., Sartoris, B., Sassolas, B., Sauniere, L., Sauvage, M., Sawicki, M., Scaramella, R., Scarlata, C., Scharré, L., Schaye, J., Schewtschenko, J. A., Schindler, J. -T., Schinnerer, E., Schirmer, M., Schmidt, F., Schmidt, M., Schneider, A., Schneider, M., Schneider, P., Schöneberg, N., Schrabback, T., Schultheis, M., Schulz, S., Schuster, N., Schwartz, J., Sciotti, D., Scodeggio, M., Scognamiglio, D., Scott, D., Scottez, V., Secroun, A., Sefusatti, E., Seidel, G., Seiffert, M., Sellentin, E., Selwood, M., Semboloni, E., Sereno, M., Serjeant, S., Serrano, S., Setnikar, G., Shankar, F., Sharples, R. M., Short, A., Shulevski, A., Shuntov, M., Sias, M., Sikkema, G., Silvestri, A., Simon, P., Sirignano, C., Sirri, G., Skottfelt, J., Slezak, E., Sluse, D., Smith, G. P., Smith, L. C., Smith, R. E., Smit, S. J. A., Soldano, F., Solheim, B. G. B., Sorce, J. G., Sorrenti, F., Soubrie, E., Spinoglio, L., Mancini, A. Spurio, Stadel, J., Stagnaro, L., Stanco, L., Stanford, S. A., Starck, J. -L., Stassi, P., Steinwagner, J., Stern, D., Stone, C., Strada, P., Strafella, F., Stramaccioni, D., Surace, C., Sureau, F., Suyu, S. H., Swindells, I., Szafraniec, M., Szapudi, I., Taamoli, S., Talia, M., Tallada-Crespí, P., Tanidis, K., Tao, C., Tarrío, P., Tavagnacco, D., Taylor, A. N., Taylor, J. E., Taylor, P. L., Teixeira, E. M., Tenti, M., Idiago, P. Teodoro, Teplitz, H. I., Tereno, I., Tessore, N., Testa, V., Testera, G., Tewes, M., Teyssier, R., Theret, N., Thizy, C., Thomas, P. D., Toba, Y., Toft, S., Toledo-Moreo, R., Tolstoy, E., Tommasi, E., Torbaniuk, O., Torradeflot, F., Tortora, C., Tosi, S., Tosti, S., Trifoglio, M., Troja, A., Trombetti, T., Tronconi, A., Tsedrik, M., Tsyganov, A., Tucci, M., Tutusaus, I., Uhlemann, C., Ulivi, L., Urbano, M., Vacher, L., Vaillon, L., Valageas, P., Valdes, I., Valentijn, E. A., Valenziano, L., Valieri, C., Valiviita, J., Broeck, M. Van den, Vassallo, T., Vavrek, R., Vega-Ferrero, J., Venemans, B., Venhola, A., Ventura, S., Kleijn, G. Verdoes, Vergani, D., Verma, A., Vernizzi, F., Veropalumbo, A., Verza, G., Vescovi, C., Vibert, D., Viel, M., Vielzeuf, P., Viglione, C., Viitanen, A., Villaescusa-Navarro, F., Vinciguerra, S., Visticot, F., Voggel, K., von Wietersheim-Kramsta, M., Vriend, W. J., Wachter, S., Walmsley, M., Walth, G., Walton, D. M., Walton, N. A., Wander, M., Wang, L., Wang, Y., Weaver, J. R., Weller, J., Wetzstein, M., Whalen, D. J., Whittam, I. H., Widmer, A., Wiesmann, M., Wilde, J., Williams, O. R., Winther, H. -A., Wittje, A., Wong, J. H. W., Wright, A. H., Yankelevich, V., Yeung, H. W., Yoon, M., Youles, S., Yung, L. Y. A., Zacchei, A., Zalesky, L., Zamorani, G., Vitorelli, A. Zamorano, Marc, M. Zanoni, Zennaro, M., Zerbi, F. M., Zinchenko, I. A., Zoubian, J., Zucca, E., and Zumalacarregui, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14,000 deg^2 of extragalactic sky. In addition to accurate weak lensing and clustering measurements that probe structure formation over half of the age of the Universe, its primary probes for cosmology, these exquisite data will enable a wide range of science. This paper provides a high-level overview of the mission, summarising the survey characteristics, the various data-processing steps, and data products. We also highlight the main science objectives and expected performance., Comment: Accepted for publication in the A&A special issue`Euclid on Sky'

Published
2024

3. Euclid Near Infrared Spectro-Photometer: spatial considerations on H2RG detectors interpixel capacitance and IPC corrected conversion gain from on-ground characterization

Author

Graët, J. Le, Secroun, A., Barbier, R., Gillard, W., Clemens, JC., Conseil, S., Escoffier, S., Ferriol, S., Fourmanoit, N., Kajfasz, E., Kermiche, S., Kubik, B., Smadja, G., and Zoubian, J.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Euclid is a major ESA mission scheduled for launch in 2023-2024 to map the geometry of the dark Universe using two primary probes, weak gravitational lensing and galaxy clustering. \Euclid's instruments, a visible imager (VIS) and an infrared spectrometer and photometer (NISP) have both been designed and built by Euclid Consortium teams. The NISP instrument will hold a large focal plane array of 16 near-infrared H2RG detectors, which are key elements to the performance of the NISP, and therefore to the science return of the mission. Euclid NISP H2RG flight detectors have been individually and thoroughly characterized at Centre de Physique des Particules de Marseille (CPPM) during a whole year with a view to producing a reference database of performance pixel maps. Analyses have been ongoing and have shown the relevance of taking into account spatial variations in deriving performance parameters. This paper will concentrate on interpixel capacitance (IPC) and conversion gain. First, per pixel IPC coefficient maps will be derived thanks to single pixel reset (SPR) measurements and a new IPC correction method will be defined and validated. Then, the paper will look into correlation effects of IPC and their impact on the derivation of per super-pixel IPC-free conversion gain maps. Eventually, several conversion gain values will be defined over clearly distinguishable regions., Comment: Comments: 1 pages, LaTeX; equation 2 corrected

Published
2022
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4. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at $1.5 < z < 6.4$

Author

Schmidt, K. B., Kerutt, J., Wisotzki, L., Urrutia, T., Feltre, A., Maseda, M. V., Nanayakkara, T., Bacon, R., Boogaard, L. A., Conseil, S., Contini, T., Herenz, E. C., Kollatschny, W., Krumpe, M., Leclercq, F., Mahler, G., Matthee, J., Mauerhofer, V., Richard, J., and Schaye, J.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

[Abbreviated] Rest-frame UV emission lines probe physical parameters of the emitting star-forming galaxies and their environments. The strongest main UV line, Ly$\alpha$, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Ly$\alpha$ emission becomes increasingly challenging at $z \gtrsim 6$ when the neutral hydrogen fraction of the CGM and IGM increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies' physical properties and their Ly$\alpha$ emission. The sample of 2052 emission line sources with $1.5 < z < 6.4$ was selected through untargeted source detection in three-dimensional MUSE data cubes. We searched optimally extracted 1D spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Ly$\alpha$) UV emission lines increases with survey depth, and that the UV emission line strength often correlate with the strength of Ciii]. We measured the velocity offsets of resonant emission lines with respect to systemic tracers as well as the electron density and the gas-phase abundance. Lastly, using "PhotoIonization Model Probability Density Functions" we find that the UV line emitters generally have ionization parameter log10(U) $\approx$ -2.5 and metal mass fractions that scatter around Z $\approx$ 10$^{-2}$, that is Z $\approx$ 0.66Z$\odot$. Value-added catalogs of the full sample of MUSE objects studied in this work and a collection of UV line emitters from the literature are provided with this paper., Comment: Accepted by A&A. Contains 54 pages, 21 figures, and appendices. Catalogs described in Tables B.1 and C.1 will be made available with published paper

Published
2021
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5. Reconstruction of the ground-layer adaptive-optics point spread function for MUSE Wide Field Mode observations

Author

Fusco, Thierry, Bacon, R., Kamann, S., Conseil, S., Neichel, Benoit, Correia, Carlos, Beltramo-Martin, Olivier, Vernet, Joel, Kolb, Johann, and Madec, Pierre-Yves

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Here we describe a simple, efficient, and most importantly fully operational point-spread-function(PSF)-reconstruction approach for laser-assisted ground layer adaptive optics (GLAO) in the frame of the Multi Unit Spectroscopic Explorer (MUSE) Wide Field Mode. Based on clear astrophysical requirements derived by the MUSE team and using the functionality of the current ESO Adaptive Optics Facility we aim to develop an operational PSF-reconstruction (PSFR) algorithm and test it both in simulations and using on-sky data. The PSFR approach is based on a Fourier description of the GLAO correction to which the specific instrumental effects of MUSE Wide Field Mode (pixel size, internal aberrations, etc.) have been added. It was first thoroughly validated with full end-to-end simulations. Sensitivity to the main atmospheric and AO system parameters was analysed and the code was re-optimised to account for the sensitivity found. Finally, the optimised algorithm was tested and commissioned using more than one year of on-sky MUSE data. We demonstrate with an on-sky data analysis that our algorithm meets all the requirements imposed by the MUSE scientists, namely an accuracy better than a few percent on the critical PSF parameters including full width at half maximum and global PSF shape through the kurtosis parameter of a Moffat function. The PSFR algorithm is publicly available and is used routinely to assess the MUSE image quality for each observation. It can be included in any post-processing activity which requires knowledge of the PSF., Comment: To be published in A&1, 14 pages, 17 figures

Published
2020
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6. The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

Author

The Astropy Collaboration, Price-Whelan, A. M., Sipőcz, B. M., Günther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Pérez-Suárez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Rodríguez, J. L. Cano, Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Crichton, D., DÁvella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezić, Ž., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Nöthe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., and Zabalza, V.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Astropy project supports and fosters the development of open-source and openly-developed Python packages that provide commonly-needed functionality to the astronomical community. A key element of the Astropy project is the core package Astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of inter-operable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy project., Comment: Minor changes to author list and title. Comments and feedback welcome through the paper source repository: https://github.com/astropy/astropy-v2.0-paper For more information about Astropy, see http://www.astropy.org/

Published
2018
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7. The MUSE Hubble Ultra Deep Field Survey VI: The Faint-End of the Lya Luminosity Function at 2.91 < z < 6.64 and Implications for Reionisation

Author

Drake, A. B., Garel, T., Wisotzki, L., Leclercq, F., Hashimoto, T., Richard, J., Bacon, R., Blaizot, J., Caruana, J., Conseil, S., Contini, T., Guiderdoni, B., Herenz, E. C., Inami, H., Lewis, J., Mahler, G., Marino, R. A., Pello, R., Schaye, J., Verhamme, A., Ventou, E., and Weilbacher, P. M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the deepest study to date of the Lya luminosity function (LF) in a blank field using blind integral field spectroscopy from MUSE. We constructed a sample of 604 Lya emitters (LAEs) across the redshift range 2.91 < z < 6.64 using automatic detection software in the Hubble Ultra Deep Field. We calculate accurate total Lya fluxes capturing low surface brightness extended Lya emission now known to be a generic property of high-redshift star-forming galaxies. We simulated realistic extended LAEs to characterise the selection function of our samples, and performed flux-recovery experiments to test and correct for bias in our determination of total Lya fluxes. We find an accurate completeness correction accounting for extended emission reveals a very steep faint-end slope of the LF, alpha, down to luminosities of log10 L erg s^-1< 41.5, applying both the 1/Vmax and maximum likelihood estimators. Splitting the sample into three broad redshift bins, we see the faint-end slope increasing from -2.03+1.42-inf at z ~ 3.44 to -2.86+0.76-inf at z ~ 5.48, however no strong evolution is seen between the 68% confidence regions in L*-alpha parameter space. Using the Lya line flux as a proxy for star formation activity, and integrating the observed LFs, we find that LAEs' contribution to the cosmic SFRD rises with redshift until it is comparable to that from continuum-selected samples by z ~ 6. This implies that LAEs may contribute more to the star-formation activity of the early Universe than previously thought - any additional interglactic medium correction would act to further boost the Lya luminosities. Finally, assuming fiducial values for the escape of Lya and LyC radiation, and the clumpiness of the IGM, we integrated the maximum likelihood LF at 5.00 < z < 6.64 and find we require only a small extrapolation beyond the data (< 1 dex in L) for LAEs alone to maintain an ionised IGM at z ~ 6., Comment: 16 pages, 10 figures. Accepted for publication in A&A special issue: "The MUSE Hubble Ultra Deep Field Survey" (MUSE UDF Series Paper VI)

Published
2017
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8. The MUSE Hubble Ultra Deep Field Survey: II. Spectroscopic redshifts and comparisons to color selections of high-redshift galaxies

Author

Inami, H., Bacon, R., Brinchmann, J., Richard, J., Contini, T., Conseil, S., Hamer, S., Akhlaghi, M., Bouche, N., Clement, B., Desprez, G., Drake, A. B., Hashimoto, T., Leclercq, F., Maseda, M., Michel-Dansac, L., Paalvast, M., Tresse, L., Ventou, E., Kollatschny, W., Boogaard, L. A., Finley, H., Marino, R. A., Schaye, J., and Wisotzki, L.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We have conducted a two-layered spectroscopic survey (1'x1' ultra deep and 3'x3' deep regions) in the Hubble Ultra Deep Field (HUDF) with the Multi Unit Spectroscopic Explorer (MUSE). The combination of a large field of view, high sensitivity, and wide wavelength coverage provides an order of magnitude improvement in spectroscopically confirmed redshifts in the HUDF; i.e., 1206 secure spectroscopic redshifts for HST continuum selected objects, which corresponds to 15% of the total (7904). The redshift distribution extends well beyond z>3 and to HST/F775W magnitudes as faint as ~30 mag (AB, 1-sigma). In addition, 132 secure redshifts were obtained for sources with no HST counterparts that were discovered in the MUSE data cubes by a blind search for emission-line features. In total, we present 1338 high quality redshifts, which is a factor of eight increase compared with the previously known spectroscopic redshifts in the same field. We assessed redshifts mainly with the spectral features [OII] at z<1.5 (473 objects) and Lya at 2.9~20% up to 28-29 mag and ~27 mag, respectively. We used the determined redshifts to test continuum color selection (dropout) diagrams of high-z galaxies. The selection condition for F336W dropouts successfully captures ~80% of the targeted z~2.7 galaxies. However, for higher redshift selections (F435W, F606W, and F775W dropouts), the success rates decrease to ~20-40%. We empirically redefine the selection boundaries to make an attempt to improve them to ~60%. The revised boundaries allow bluer colors that capture Lya emitters with high Lya equivalent widths falling in the broadbands used for the color-color selection. Along with this paper, we release the redshift and line flux catalog., Comment: 26 pages, 26 figures, 4 tables, accepted for publication in A&A (MUSE UDF Series Paper II), the redshift catalogs will be available at the CDS

Published
2017
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9. The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package* * The author list has three parts: the authors that made significant contributions to the writing of the paper in order of contribution, the four members of the Astropy Project coordination committee, and contributors to the Astropy Project in alphabetical order. Their position in the author list does not correspond to contributions to the Astropy Project as a whole. A more complete list of contributors to the core package can be found in the package repository and at the Astropy team webpage.

Author

Price-Whelan, AM, Sipőcz, BM, Günther, HM, Lim, PL, Crawford, SM, Conseil, S, Shupe, DL, Craig, MW, Dencheva, N, Ginsburg, A, VanderPlas, JT, Bradley, LD, Pérez-Suárez, D, de Val-Borro, M, Aldcroft, TL, Cruz, KL, Robitaille, TP, Tollerud, EJ, Ardelean, C, Babej, T, Bach, YP, Bachetti, M, Bakanov, AV, Bamford, SP, Barentsen, G, Barmby, P, Baumbach, A, Berry, KL, Biscani, F, Boquien, M, Bostroem, KA, Bouma, LG, Brammer, GB, Bray, EM, Breytenbach, H, Buddelmeijer, H, Burke, DJ, Calderone, G, Rodríguez, JL Cano, Cara, M, Cardoso, JVM, Cheedella, S, Copin, Y, Corrales, L, Crichton, D, D’Avella, D, Deil, C, Depagne, É, Dietrich, JP, Donath, A, Droettboom, M, Earl, N, Erben, T, Fabbro, S, Ferreira, LA, Finethy, T, Fox, RT, Garrison, LH, Gibbons, SLJ, Goldstein, DA, Gommers, R, Greco, JP, Greenfield, P, Groener, AM, Grollier, F, Hagen, A, Hirst, P, Homeier, D, Horton, AJ, Hosseinzadeh, G, Hu, L, Hunkeler, JS, Ivezić, Ž, Jain, A, Jenness, T, Kanarek, G, Kendrew, S, Kern, NS, Kerzendorf, WE, Khvalko, A, King, J, Kirkby, D, Kulkarni, AM, Kumar, A, Lee, A, Lenz, D, Littlefair, SP, Ma, Z, Macleod, DM, Mastropietro, M, McCully, C, Montagnac, S, Morris, BM, Mueller, M, Mumford, SJ, Muna, D, Murphy, NA, Nelson, S, Nguyen, GH, and Ninan, JP

Subjects
methods: data analysis, methods: miscellaneous, methods: statistical, reference systems, astro-ph.IM, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.

Published
2018

10. The VIPERS Multi-Lambda Survey. I. UV and NIR Observations, multi-color catalogues and photometric redshifts

Author

Moutard, T., Arnouts, S., Ilbert, O., Coupon, J., Hudelot, P., Vibert, D., Comte, V., Conseil, S., Davidzon, I., Guzzo, L., Llebaria, A., Martin, C., McCracken, H. J., Milliard, B., Morrison, G. E., Schiminovich, D., Treyer, M., and Van Werbaeke, L.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present observations collected in the CFHTLS-VIPERS region in the ultraviolet (UV) with the GALEX satellite (far and near UV channels) and the near infrared with the CFHT/WIRCam camera ($K_s$-band) over an area of 22 and 27 deg$^2$, respectively. The depth of the photometry was optimized to measure the physical properties (e.g., SFR, stellar masses) of all the galaxies in the VIPERS spectroscopic survey. The large volume explored by VIPERS will enable a unique investigation of the relationship between the galaxy properties and their environment (density field and cosmic web) at high redshift (0.5 < z < 1.2). In this paper, we present the observations, the data reductions and the build-up of the multi-color catalogues. The CFHTLS-T0007 (gri-{\chi}^2) images are used as reference to detect and measure the $K_s$-band photometry, while the T0007 u-selected sources are used as priors to perform the GALEX photometry based on a dedicated software (EMphot). Our final sample reaches $NUV_{AB}$~25 (at 5{\sigma}) and $K_{AB}$~22 (at 3{\sigma}). The large spectroscopic sample (~51,000 spectroscopic redshifts) allows us to highlight the robustness of our star/galaxy separation, and the reliability of our photometric redshifts with a typical accuracy $\sigma_z \le$ 0.04 and a catastrophic failure rate {\eta} < 2% down to i~23. We present various tests on the $K_s$ band completeness and photometric redshift accuracy by comparing with existing, overlapping deep photometric catalogues. Finally, we discuss the BzK sample of passive and active galaxies at high redshift and the evolution of galaxy morphology in the (NUV-r) vs (r-K_s) diagram at low redshift (z < 0.25) thanks to the high image quality of the CFHTLS. The images, catalogues and photometric redshifts for 1.5 million sources (down to $NUV \le$ 25 or $K_s \le$ 22) are released and available at this URL: http://cesam.lam.fr/vipers-mls/, Comment: 14 pages, 16 figures. Accepted for publication in A&A. Version to be published

Published
2016
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11. Euclid commissioning results: the near infrared spectrometer and photometer (NISP) signal detection chain

Author

E. Coyle, Laura, Matsuura, Shuji, D. Perrin, Marshall, Cogato, F., Villegas, E. Medinaceli, Barbier, R., Dusini, S., Gillard, W., Jahnke, K., Auricchio, N., Balbi, E., Balestra, A., Battaglia, P., Bonino, D., Capobianco, V., Chary, R., Conseil, S., Corcione, L., Delucchi, G., Farinelli, R., Ferriol, S., Franceschi, E., Gabarra, L., Gianotti, F., Grupp, F., Lentini, E., Ligori, S., Morgante, G., Paterson, K., Romelli, E., Sauniere, L., Schirmer, M., Sirignaro, C., Sirri, G., Testera, G., Trifoglio, M., Troja, A., Valenziano, L., Copin, Y., Frailis, M., Kubik, B., Scodeggio, M., Barriere, J.-C., Berthe, M., Bodendorf, C., Caillat, A., Carle, M., Casas, R., Cho, H., Costille, A., Ducret, F., Garilli, B., Holmes, W., Hormuth, F., Hornstrup, A., Jhabvala, M., Kohley, R., Mignant, D. Le, Lilje, P. B., Lloro, I., Padilla, C., Polenta, G., Salvignol, J.-C., Seidel, G., Serra, B., Secroun, A., Smadja, G., Stanco, L., Strada, P., Toledo-Moreo, R., Anselmi, S., Borsato, E., Caillat, L., Colodro-Conde, C., Conforti, V., Davies, J., Renzi, A., Corso, F. Dal, Davini, S., Rosa, A. De, Diaz, J., Domizio, S. Di, Ferdinando, D. Di, Ferrari, A., Fornari, F., Giacomini, F., Krause, O., Laudisio, F., Macias-Perez, J., Marpaud, J., Mauri, N., Silva, R. da, Niclas, M., Passalacqua, F., Risso, I., Lagier, P., Sorensen, A. N., Stassi, P., Steinwagner, J., Tenti, M., Thizy, C., Tosi, S., Travaglini, R., Tubio, O., Valieri, C., Ventura, S., Vescovi, C., Zoubian, J., E. Coyle, Laura, Matsuura, Shuji, D. Perrin, Marshall, Cogato, F., Villegas, E. Medinaceli, Barbier, R., Dusini, S., Gillard, W., Jahnke, K., Auricchio, N., Balbi, E., Balestra, A., Battaglia, P., Bonino, D., Capobianco, V., Chary, R., Conseil, S., Corcione, L., Delucchi, G., Farinelli, R., Ferriol, S., Franceschi, E., Gabarra, L., Gianotti, F., Grupp, F., Lentini, E., Ligori, S., Morgante, G., Paterson, K., Romelli, E., Sauniere, L., Schirmer, M., Sirignaro, C., Sirri, G., Testera, G., Trifoglio, M., Troja, A., Valenziano, L., Copin, Y., Frailis, M., Kubik, B., Scodeggio, M., Barriere, J.-C., Berthe, M., Bodendorf, C., Caillat, A., Carle, M., Casas, R., Cho, H., Costille, A., Ducret, F., Garilli, B., Holmes, W., Hormuth, F., Hornstrup, A., Jhabvala, M., Kohley, R., Mignant, D. Le, Lilje, P. B., Lloro, I., Padilla, C., Polenta, G., Salvignol, J.-C., Seidel, G., Serra, B., Secroun, A., Smadja, G., Stanco, L., Strada, P., Toledo-Moreo, R., Anselmi, S., Borsato, E., Caillat, L., Colodro-Conde, C., Conforti, V., Davies, J., Renzi, A., Corso, F. Dal, Davini, S., Rosa, A. De, Diaz, J., Domizio, S. Di, Ferdinando, D. Di, Ferrari, A., Fornari, F., Giacomini, F., Krause, O., Laudisio, F., Macias-Perez, J., Marpaud, J., Mauri, N., Silva, R. da, Niclas, M., Passalacqua, F., Risso, I., Lagier, P., Sorensen, A. N., Stassi, P., Steinwagner, J., Tenti, M., Thizy, C., Tosi, S., Travaglini, R., Tubio, O., Valieri, C., Ventura, S., Vescovi, C., and Zoubian, J.

Abstract

Euclid, the M2 mission of the ESA’s Cosmic Vision 2015-2025 program, aims to explore the Dark Universe by conducting a survey of approximately 14 000 deg2 and creating a 3D map of the observable Universe of around 1.5 billion galaxies up to redshift z ∼ 2. This mission uses two main cosmological probes: weak gravitational lensing and galaxy clustering, leveraging the high-resolution imaging capabilities of the Visual Imaging (VIS) instrument and the photometric and spectroscopic measurements of the Near Infrared Spectrometer and Photometer (NISP) instrument. This paper details some of the activities performed during the commissioning phase of the NISP instrument, following the launch of Euclid on July 1, 2023. In particular, we focus on the calibration of the NISP detectors’ baseline and on the performance of a parameter provided by the onboard data processing (called NISP Quality Factor, QF) in detecting the variability of the flux of cosmic rays hitting the NISP detectors. The NISP focal plane hosts sixteen Teledyne HAWAII-2RG (H2RG) detectors. The calibration of these detectors includes the baseline optimization, which optimizes the dynamic range and stability of the signal acquisition. Additionally, this paper investigates the impact of Solar proton flux on the NISP QF, particularly during periods of high Solar activity. Applying a selection criterion on the QF (called NISP QF Proxy), the excess counts are used to monitor the amount of charged particles hitting the NISP detectors. A good correlation was found between the Solar proton flux component above 30 MeV and the NISP QF Proxy, revealing that NISP detectors are not subject to the lower energy components, which are absorbed by the shielding provided by the spacecraft.

Published
2024

12. DRAGONS—A Quick Overview

Author

Labrie, K., primary, Simpson, C., additional, Cardenes, R., additional, Turner, J., additional, Soraisam, M., additional, Quint, B., additional, Oberdorf, O., additional, Placco, V. M., additional, Berke, D., additional, Smirnova, O., additional, Conseil, S., additional, Vacca, W. D., additional, and Thomas-Osip, J., additional

Published
2023
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13. Euclid commissioning results: the near infrared spectrometer and photometer (NISP) signal detection chain

Author

Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Cogato, F., Medinaceli Villegas, E., Barbier, R., Dusini, S., Gillard, W., Jahnke, K., Auricchio, N., Balbi, E., Balestra, A., Battaglia, P., Bonino, D., Capobianco, V., Chary, R., Conseil, S., Corcione, L., Delucchi, G., Farinelli, R., Ferriol, S., Franceschi, E., Gabarra, L., Gianotti, F., Grupp, F., Lentini, E., Ligori, S., Morgante, G., Paterson, K., Romelli, E., Sauniere, L., Schirmer, M., Sirignaro, C., Sirri, G., Testera, G., Trifoglio, M., Troja, A., Valenziano, L., Copin, Y., Frailis, M., Kubik, B., Scodeggio, M., Barriere, J.-C., Berthe, M., Bodendorf, C., Caillat, A., Carle, M., Casas, R., Cho, H., Costille, A., Ducret, F., Garilli, B., Holmes, W., Hormuth, F., Hornstrup, A., Jhabvala, M., Kohley, R., Le Mignant, D., Lilje, P. B., Lloro, I., Padilla, C., Polenta, G., Salvignol, J.-C., Seidel, G., Serra, B., Secroun, A., Smadja, G., Stanco, L., Strada, P., Toledo-Moreo, R., Anselmi, S., Borsato, E., Caillat, L., Colodro-Conde, C., Conforti, V., Davies, J., Renzi, A., Dal Corso, F., Davini, S., De Rosa, A., Diaz, J., Di Domizio, S., Di Ferdinando, D., Ferrari, A., Fornari, F., Giacomini, F., Krause, O., Laudisio, F., Macias-Perez, J., Marpaud, J., Mauri, N., da Silva, R., Niclas, M., Passalacqua, F., Risso, I., Lagier, P., Sorensen, A. N., Stassi, P., Steinwagner, J., Tenti, M., Thizy, C., Tosi, S., Travaglini, R., Tubio, O., Valieri, C., Ventura, S., Vescovi, C., and Zoubian, J.

Published
2024
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14. Euclid: the near infrared spectrometer and photometer (NISP) instrument operations

Author

Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Battaglia, P., Sirignano, C., Dusini, S., Gregorio, A., Ligori, S., Medinaceli, E., Romelli, E., Zacchei, A., Barbier, R., Gillard, W., Copin, Y., Jahnke, K., Schirmer, M., Auricchio, N., Balbi, E., Balestra, A., Bonino, D., Borsato, E., Brescia, M., Capobianco, V., Cavuoti, S., Cogato, F., Conseil, S., Corcione, L., Davini, S., Delucchi, G., Farinelli, R., Franceschi, E., Grupp, F., Kubik, B., Lentini, E., Lhoussaine, R., Maciaszek, T., Morgante, G., Passalacqua, F., Polenta, G., Riccio, G., Testera, G., Tosi, S., Trifoglio, M., Troja, A., and Valenziano, L.

Published
2024
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15. The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package*

Author

Zonca, A, Price-Whelan, AM, Lim, PL, Earl, N, Starkman, N, Bradley, L, Shupe, DL, Patil, AA, Corrales, L, Brasseur, CE, Nöthe, M, Donath, A, Tollerud, E, Morris, BM, Ginsburg, A, Vaher, E, Weaver, BA, Tocknell, J, Jamieson, W, Van Kerkwijk, MH, Robitaille, TP, Merry, B, Bachetti, M, Günther, HM, Zhang, C, Aldcroft, TL, Alvarado-Montes, JA, Archibald, AM, Bódi, A, Bapat, S, Barentsen, G, Bazán, J, Biswas, M, Boquien, M, Burke, DJ, Cara, D, Cara, M, Conroy, KE, Conseil, S, Craig, MW, Cross, RM, Cruz, KL, D’Eugenio, F, Dencheva, N, Devillepoix, HAR, Dietrich, JP, Eigenbrot, AD, Erben, T, Ferreira, L, Foreman-Mackey, D, Fox, R, Freij, N, Garg, S, Geda, R, Glattly, L, Gondhalekar, Y, Gordon, KD, Grant, D, Greenfield, P, Groener, AM, Guest, S, Gurovich, S, Handberg, R, Hart, A, Hatfield-Dodds, Z, Homeier, D, Hosseinzadeh, G, Jenness, T, Jones, CK, Joseph, P, Kalmbach, JB, Karamehmetoglu, E, Kałuszyński, M, Kelley, MSP, Kern, N, Kerzendorf, WE, Koch, EW, Kulumani, S, Lee, A, Ly, C, Ma, Z, MacBride, C, Maljaars, JM, Muna, D, Murphy, NA, Norman, H, O’Steen, R, Oman, KA, Pacifici, C, Pascual, S, Pascual-Granado, J, Patil, RR, Perren, GI, Pickering, TE, Rastogi, T, Roulston, BR, Ryan, DF, Rykoff, ES, Sabater, J, Sakurikar, P, Zonca, A [0000-0001-6841-1058], Price-Whelan, AM [0000-0003-0872-7098], Lim, PL [0000-0003-0079-4114], Earl, N [0000-0003-1714-7415], Starkman, N [0000-0003-3954-3291], Bradley, L [0000-0002-7908-9284], Shupe, DL [0000-0003-4401-0430], Patil, AA [0000-0002-7626-506X], Corrales, L [0000-0002-5466-3817], Brasseur, CE [0000-0002-9314-960X], Nöthe, M [0000-0001-7993-8189], Donath, A [0000-0003-4568-7005], Tollerud, E [0000-0002-9599-310X], Morris, BM [0000-0003-2528-3409], Ginsburg, A [0000-0001-6431-9633], Vaher, E [0000-0001-8736-1762], Tocknell, J [0000-0001-6637-6922], Jamieson, W [0000-0001-5976-4492], van Kerkwijk, MH [0000-0002-5830-8505], Robitaille, TP [0000-0002-8642-1329], Bachetti, M [0000-0002-4576-9337], Günther, HM [0000-0003-4243-2840], Zhang, C [0000-0002-9583-263X], Alvarado-Montes, JA [0000-0003-0353-9741], Archibald, AM [0000-0003-0638-3340], Bódi, A [0000-0002-8585-4544], Bapat, S [0000-0002-0870-4665], Barentsen, G [0000-0002-3306-3484], Bazán, J [0000-0001-7699-3983], Boquien, M [0000-0003-0946-6176], Burke, DJ [0000-0003-4428-7835], Cara, D [0000-0003-3833-1668], Cara, M [0000-0002-9294-6551], Conroy, KE [0000-0002-5442-8550], Conseil, S [0000-0002-3657-4191], Craig, MW [0000-0001-7988-8919], Cross, RM [0000-0003-0081-8024], Cruz, KL [0000-0002-1821-0650], D’Eugenio, F [0000-0003-2388-8172], Dencheva, N [0000-0002-5686-9632], Devillepoix, HAR [0000-0001-9226-1870], Dietrich, JP [0000-0002-8134-9591], Eigenbrot, AD [0000-0003-0810-4368], Ferreira, L [0000-0002-8919-079X], Foreman-Mackey, D [0000-0002-9328-5652], Freij, N [0000-0002-6253-082X], Garg, S [0000-0002-2309-9731], Geda, R [0000-0003-1509-9966], Gondhalekar, Y [0000-0002-6646-4225], Gordon, KD [0000-0001-5340-6774], Grant, D [0000-0001-5878-618X], Greenfield, P [0000-0003-2269-0551], Groener, AM [0000-0002-6508-2938], Gurovich, S [0000-0001-5848-4077], Handberg, R [0000-0001-8725-4502], Hart, A [0000-0002-8138-1479], Hatfield-Dodds, Z [0000-0002-8646-8362], Homeier, D [0000-0002-8546-9128], Hosseinzadeh, G [0000-0002-0832-2974], Jenness, T [0000-0001-5982-167X], Jones, CK [0000-0002-0629-3006], Joseph, P [0000-0003-1409-1903], Kalmbach, JB [0000-0002-6825-5283], Karamehmetoglu, E [0000-0001-6209-838X], Kałuszyński, M [0000-0003-0109-5833], Kelley, MSP [0000-0002-6702-7676], Kern, N [0000-0002-8211-1892], Kerzendorf, WE [0000-0002-0479-7235], Koch, EW [0000-0001-9605-780X], Kulumani, S [0000-0002-7822-0471], Lee, A [0000-0003-2193-5369], Ly, C [0000-0002-4245-2318], Ma, Z [0000-0003-3270-6844], MacBride, C [0000-0002-9901-8723], Maljaars, JM [0000-0001-8100-9514], Muna, D [0000-0002-1631-4114], Murphy, NA [0000-0001-6628-8033], Norman, H [0000-0003-4189-3450], O’Steen, R [0000-0002-2432-8946], Oman, KA [0000-0001-9857-7788], Pacifici, C [0000-0003-4196-0617], Pascual, S [0000-0002-9351-6051], Pascual-Granado, J [0000-0003-0139-6951], Patil, RR [0000-0002-5923-4966], Perren, GI [0000-0002-1852-9653], Pickering, TE [0000-0002-9427-5448], Roulston, BR [0000-0002-9453-7735], Ryan, DF [0000-0001-8661-3825], Rykoff, ES [0000-0001-9376-3135], Sabater, J [0000-0003-1149-6294], Sakurikar, P [0000-0002-9523-5640], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 5109 Space Sciences, 51 Physical Sciences, 5107 Particle and High Energy Physics
Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we summarize key features in the core package as of the recent major release, version 5.0, and provide major updates on the Project. We then discuss supporting a broader ecosystem of interoperable packages, including connections with several astronomical observatories and missions. We also revisit the future outlook of the Astropy Project and the current status of Learn Astropy. We conclude by raising and discussing the current and future challenges facing the Project.

Published
2022

16. Three Dimensional Fingertip Tracking in Stereovision

Author

Conseil, S., Bourennane, S., Martin, L., Hutchison, David, editor, Kanade, Takeo, editor, Kittler, Josef, editor, Kleinberg, Jon M., editor, Mattern, Friedemann, editor, Mitchell, John C., editor, Naor, Moni, editor, Nierstrasz, Oscar, editor, Pandu Rangan, C., editor, Steffen, Bernhard, editor, Sudan, Madhu, editor, Terzopoulos, Demetri, editor, Tygar, Dough, editor, Vardi, Moshe Y., editor, Weikum, Gerhard, editor, Blanc-Talon, Jacques, editor, Philips, Wilfried, editor, Popescu, Dan, editor, and Scheunders, Paul, editor

Published
2005
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17. Efficiently combining α CenA multi-epoch high-contrast imaging data

Author

Le Coroller, H., primary, Nowak, M., additional, Wagner, K., additional, Kasper, M., additional, Chauvin, G., additional, Desgrange, C., additional, Conseil, S., additional, Jakob, G., additional, Käufl, U., additional, Leveratto, S., additional, Pantin, E., additional, Siebenmorgen, R., additional, and Arsenault, R., additional

Published
2022
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18. Euclid Near Infrared Spectro-Photometer: spatial considerations on H2RG detectors interpixel capacitance and IPC corrected conversion gain from on-ground characterization

Author

Le Graët, J., Secroun, A., Barbier, R., Gillard, W., Clémens, J.-C., Conseil, S., Escoffier, S., Ferriol, S., Fourmanoit, N., Kajfasz, E., Kermiche, S., Kubik, B., Smadja, G., Zoubian, J., Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

International audience; Euclid is a major ESA mission scheduled for launch in 2023-2024 to map the geometry of the dark Universe using two primary probes, weak gravitational lensing and galaxy clustering. \Euclid's instruments, a visible imager (VIS) and an infrared spectrometer and photometer (NISP) have both been designed and built by Euclid Consortium teams. The NISP instrument will hold a large focal plane array of 16 near-infrared H2RG detectors, which are key elements to the performance of the NISP, and therefore to the science return of the mission. Euclid NISP H2RG flight detectors have been individually and thoroughly characterized at Centre de Physique des Particules de Marseille (CPPM) during a whole year with a view to producing a reference database of performance pixel maps. Analyses have been ongoing and have shown the relevance of taking into account spatial variations in deriving performance parameters. This paper will concentrate on interpixel capacitance (IPC) and conversion gain. First, per pixel IPC coefficient maps will be derived thanks to single pixel reset (SPR) measurements and a new IPC correction method will be defined and validated. Then, the paper will look into correlation effects of IPC and their impact on the derivation of per super-pixel IPC-free conversion gain maps. Eventually, several conversion gain values will be defined over clearly distinguishable regions.

Published
2022
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19. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < 6.4

Author

Schmidt, K. B., primary, Kerutt, J., additional, Wisotzki, L., additional, Urrutia, T., additional, Feltre, A., additional, Maseda, M. V., additional, Nanayakkara, T., additional, Bacon, R., additional, Boogaard, L. A., additional, Conseil, S., additional, Contini, T., additional, Herenz, E. C., additional, Kollatschny, W., additional, Krumpe, M., additional, Leclercq, F., additional, Mahler, G., additional, Matthee, J., additional, Mauerhofer, V., additional, Richard, J., additional, and Schaye, J., additional

Published
2021
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20. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift

Author

Bacon, R., primary, Mary, D., additional, Garel, T., additional, Blaizot, J., additional, Maseda, M., additional, Schaye, J., additional, Wisotzki, L., additional, Conseil, S., additional, Brinchmann, J., additional, Leclercq, F., additional, Abril-Melgarejo, V., additional, Boogaard, L., additional, Bouché, N. F., additional, Contini, T., additional, Feltre, A., additional, Guiderdoni, B., additional, Herenz, C., additional, Kollatschny, W., additional, Kusakabe, H., additional, Matthee, J., additional, Michel-Dansac, L., additional, Nanayakkara, T., additional, Richard, J., additional, Roth, M., additional, Schmidt, K. B., additional, Steinmetz, M., additional, Tresse, L., additional, Urrutia, T., additional, Verhamme, A., additional, Weilbacher, P. M., additional, Zabl, J., additional, and Zoutendijk, S. L., additional

Published
2021
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22. Ground Layer Adaptive Optics Point Spread Function reconstruction for MUSE Wide Field mode observations

Author

Fusco, Thierry, Bacon, Roland, Kamann, Sebastian, Conseil, S., Neichel, Benoit, Correia, Carlos, Beltramo-Martin, Olivier, Vernet, Joel, Kolb, Johann, Madec, Pierre-Yves, DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and European Southern Observatory (ESO)

Subjects
[PHYS]Physics [physics], [SPI]Engineering Sciences [physics]
Abstract

International audience; Context. This paper describes a simple, efficient and most importantly fully operational Point Spread Function (PSF) reconstruction approach for Laser assisted Ground Layer Adaptive Optics (GLAO) in the frame of the MUSE Wide Field Mode. Aims. Based on clear astrophysical requirements derived by the MUSE team and using the current ESO Adaptive Optics Facility functionalities an operational PSF Reconstruction (PSFR) algorithm has been developed and tested in simulations and using on-sky data. Methods. The PSFR approach is based on a Fourier description of the GLAO correction on which the specific instrumental effects of MUSE Wide Field Mode (pixel size, internal aberrations ...) have been added. It has been first thorough validated with full end-to-end simulations. Sensitivity to the main atmospheric and AO system parameters has been analyzed and the code has been re-optimised to account for this analysis. Finally the optimized algorithm has been tested and commissioned using more than one year of on-sky MUSE data Results. We demonstrate with on-sky data analysis that our algorithm meets all the requirements imposed by the MUSE scientists: an accuracy better than a few percent on the critical PSF parameters including Full Width Half Maximum and global PSF shape through the kurtosis parameter of a Moffat function. Conclusions. The PSFR algorithm is publicly available and is used routinely to assess the MUSE image quality for each observation and can be included in any post processing activity which requires a knowledge of the PSF.

Published
2020
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25. The Astropy Project: building an open-science project and status of the v2.0 core package

Author

Price-Whelan, A.M., Sip?cz, B.M., Lim, P.L., Crawford, S.M., Conseil, S., Shupe, D.L., Craig, M.W., Dencheva, N., Ginsburg, A., VanderPlas, J.T., Bradley, L.D., de Val-Borro, M., Aldcroft, T.L., Cruz, K.L., Robitaille, T.P., Tollerud, E.J., and Bamford, S.P.

Subjects
data analysis – methods: miscellaneous, methods: statistical – reference systems
Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.

Published
2018

26. The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package

Author

Collaboration, A., Price-Whelan, A., Sipőcz, B., Günther, H., Lim, P., Crawford, S., Conseil, S., Shupe, D., Craig, M., Dencheva, N., Ginsburg, A., VanderPlas, J., Bradley, L., Pérez-Suárez, D., de Val-Borro, M., Aldcroft, T., Cruz, K., Robitaille, T., Tollerud, E., Ardelean, C., Babej, T., Bach, Y., Bachetti, M., Bakanov, A., Bamford, S., Barentsen, G., Barmby, P., Baumbach, A., Berry, K., Biscani, F., Boquien, M., Bostroem, K., Bouma, L., Brammer, G., Bray, E., Breytenbach, H., Buddelmeijer, H., Burke, D., Calderone, G., Cano Rodríguez, J., Cara, M., Cardoso, J., Cheedella, S., Copin, Y., Corrales, L., Crichton, D., D'Avella, D., Deil, C., Depagne, É., Dietrich, J., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L., Finethy, T., Fox, R., Garrison, L., Gibbons, S., Goldstein, D., Gommers, R., Greco, J., Greenfield, P., Groener, A., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A., Hosseinzadeh, G., Hu, L., Hunkeler, J., Ivezić, Ž., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N., Kerzendorf, W., Khvalko, A., King, J., Kirkby, D., Kulkarni, A., Kumar, A., Lee, A., Lenz, D., Littlefair, S., Ma, Z., Macleod, D., Mastropietro, M., McCully, C., Montagnac, S., Morris, B., Mueller, M., Mumford, S., Muna, D., Murphy, N., Nelson, S., Nguyen, G., Ninan, J., Nöthe, M., Ogaz, S., Oh, S., Parejko, J., Parley, N., Pascual, S., Patil, R., Patil, A., Plunkett, A., Prochaska, J., Rastogi, T., Reddy Janga, V., Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L., Sherwood-Taylor, H., Shih, A., Sick, J., Silbiger, M., Singanamalla, S., Singer, L., Sladen, P., Sooley, K., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S., Tremblay, G., Turner, J., Terrón, V., van Kerkwijk, M., de la Vega, A., Watkins, L., Weaver, B., Whitmore, J., Woillez, J., Zabalza, V., Contributors, A., Centre de Recherche Astrophysique de Lyon (CRAL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Google, NumFOCUS, Space Telescope Science Institute (US), Harvard-Smithsonian Center for Astrophysics, South African Astronomical Observatory, National Aeronautics and Space Administration (US), Gordon and Betty Moore Foundation, Alfred P. Sloan Foundation, Washington Research Foundation, German Research Foundation, Gemini Observatory, Korea Astronomy and Space Science Institute, Ministerio de Economía y Competitividad (España), European Commission, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astropy, and Physics

Subjects
methods: statistical, Engineering, Open science, 010308 nuclear & particles physics, business.industry, statistical [methods], Astronomy and Astrophysics, Python (programming language), Key features, methods: data analysis, 01 natural sciences, Engineering management, Space and Planetary Science, methods: miscellaneous, 0103 physical sciences, data analysis [methods], reference systems, [INFO]Computer Science [cs], miscellaneous [methods], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, 010303 astronomy & astrophysics, computer, computer.programming_language
Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.© 2018. The American Astronomical Society., The Astropy community is supported by and makes use of a number of organizations and services outside the traditional academic community. We thank Google for financing and organizing the Google Summer of Code (GSoC) program, that has funded several students per year to work on Astropy related projects over the summer. These students often turn into longterm contributors. We also thank NumFOCUS and the Python Software Foundation for financial support. Within the academic community, we thank institutions that make it possible for astronomers and other developers on their staff to contribute their time to the development of Astropy projects. We acknowledge the support of the Space Telescope Science Institute, Harvard-Smithsonian Center for Astrophysics, and the South African Astronomical Observatory.r The following individuals would like to recognize support for their personal contributions. H.M.G. was supported by the National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for Support of the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. J.T.V. was supported by the UW eScience Institute via grants from the Moore Foundation, the Sloan Foundation, and the Washington Research Foundation. S.M.C. acknowledges the National Research Foundation of South Africa. M.V.B. was supported by NASA's Planetary Astronomy Program. T.L.A. was supported by NASA contract NAS8-03060. Support for E.J.T. was provided by NASA through Hubble Fellowship grant No. 51316.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555, as well as a Giacconi Fellowship. M.B. was supported by the FONDECYT regular project 1170618 and the MINEDUC-UA projects codes ANT 1655 and ANT 1656. D.H. was supported through the SFB 881 >The Milky Way System> by the German Research Foundation (DFG). W.E.K was supported by an ESO Fellowship. C.M. is supported by NSF grant AST-1313484. S.P. was supported by grant AYA2016-75808-R (FEDER) issued by the Spanish government. J.E.H.T. was supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Brazil, Canada, Chile, and the United States of America. Y.P.B was supported by the Korea Astronomy and Space Science Institute, under the R&D program supervised by the Ministry of Science, ICT, and Future Planning.

Published
2018
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28. The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package

Author

Price-Whelan, AM, Price-Whelan, AM, Sipõcz, BM, Günther, HM, Lim, PL, Crawford, SM, Conseil, S, Shupe, DL, Craig, MW, Dencheva, N, Ginsburg, A, Vanderplas, JT, Bradley, LD, Pérez-Suárez, D, De Val-Borro, M, Aldcroft, TL, Cruz, KL, Robitaille, TP, Tollerud, EJ, Ardelean, C, Babej, T, Bach, YP, Bachetti, M, Bakanov, AV, Bamford, SP, Barentsen, G, Barmby, P, Baumbach, A, Berry, KL, Biscani, F, Boquien, M, Bostroem, KA, Bouma, LG, Brammer, GB, Bray, EM, Breytenbach, H, Buddelmeijer, H, Burke, DJ, Calderone, G, Rodríguez, JLC, Cara, M, Cardoso, JVM, Cheedella, S, Copin, Y, Corrales, L, Crichton, D, D'Avella, D, Deil, C, Depagne, Dietrich, JP, Donath, A, Droettboom, M, Earl, N, Erben, T, Fabbro, S, Ferreira, LA, Finethy, T, Fox, RT, Garrison, LH, Gibbons, SLJ, Goldstein, DA, Gommers, R, Greco, JP, Greenfield, P, Groener, AM, Grollier, F, Hagen, A, Hirst, P, Homeier, D, Horton, AJ, Hosseinzadeh, G, Hu, L, Hunkeler, JS, Ivezić, Jain, A, Jenness, T, Kanarek, G, Kendrew, S, Kern, NS, Kerzendorf, WE, Khvalko, A, King, J, Kirkby, D, Kulkarni, AM, Kumar, A, Lee, A, Lenz, D, Littlefair, SP, Ma, Z, MacLeod, DM, Mastropietro, M, McCully, C, Montagnac, S, Morris, BM, Mueller, M, Mumford, SJ, Muna, D, Murphy, NA, Nelson, S, Nguyen, GH, Ninan, JP, Price-Whelan, AM, Price-Whelan, AM, Sipõcz, BM, Günther, HM, Lim, PL, Crawford, SM, Conseil, S, Shupe, DL, Craig, MW, Dencheva, N, Ginsburg, A, Vanderplas, JT, Bradley, LD, Pérez-Suárez, D, De Val-Borro, M, Aldcroft, TL, Cruz, KL, Robitaille, TP, Tollerud, EJ, Ardelean, C, Babej, T, Bach, YP, Bachetti, M, Bakanov, AV, Bamford, SP, Barentsen, G, Barmby, P, Baumbach, A, Berry, KL, Biscani, F, Boquien, M, Bostroem, KA, Bouma, LG, Brammer, GB, Bray, EM, Breytenbach, H, Buddelmeijer, H, Burke, DJ, Calderone, G, Rodríguez, JLC, Cara, M, Cardoso, JVM, Cheedella, S, Copin, Y, Corrales, L, Crichton, D, D'Avella, D, Deil, C, Depagne, Dietrich, JP, Donath, A, Droettboom, M, Earl, N, Erben, T, Fabbro, S, Ferreira, LA, Finethy, T, Fox, RT, Garrison, LH, Gibbons, SLJ, Goldstein, DA, Gommers, R, Greco, JP, Greenfield, P, Groener, AM, Grollier, F, Hagen, A, Hirst, P, Homeier, D, Horton, AJ, Hosseinzadeh, G, Hu, L, Hunkeler, JS, Ivezić, Jain, A, Jenness, T, Kanarek, G, Kendrew, S, Kern, NS, Kerzendorf, WE, Khvalko, A, King, J, Kirkby, D, Kulkarni, AM, Kumar, A, Lee, A, Lenz, D, Littlefair, SP, Ma, Z, MacLeod, DM, Mastropietro, M, McCully, C, Montagnac, S, Morris, BM, Mueller, M, Mumford, SJ, Muna, D, Murphy, NA, Nelson, S, Nguyen, GH, and Ninan, JP

Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.

Published
2018

29. The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package

Author

Physics, Price-Whelan, A. M., Sipocz, B. M., Gunther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Perez-Suarez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Cano Rodriguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Crichton, D., D'Avella, D., Deil, C., Depagne, E., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezic, Z., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Noethe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terron, V., van Kerkwijk, M. H., de la Vegat, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., Physics, Price-Whelan, A. M., Sipocz, B. M., Gunther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., VanderPlas, J. T., Bradley, L. D., Perez-Suarez, D., de Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Cano Rodriguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Crichton, D., D'Avella, D., Deil, C., Depagne, E., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezic, Z., Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Noethe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Janga, V. Reddy, Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terron, V., van Kerkwijk, M. H., de la Vegat, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., and Zabalza, V.

Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.

Published
2018

30. The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package

Author

Google, NumFOCUS, Space Telescope Science Institute (US), Harvard-Smithsonian Center for Astrophysics, South African Astronomical Observatory, National Aeronautics and Space Administration (US), Gordon and Betty Moore Foundation, Alfred P. Sloan Foundation, Washington Research Foundation, German Research Foundation, Gemini Observatory, Korea Astronomy and Space Science Institute, Ministerio de Economía y Competitividad (España), European Commission, Price-Whelan, Adrian M., Sipőcz, B. M., Günther, H.M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, Adam, VanderPlas, J. T., Burke, D. J., Calderone, G., Cano Rodríguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Groener, A. M., Crichton, D., Jenness, T., D'Avella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Grollier, F., Kanarek, G., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Hagen, A., Hirst, P., Kendrew, S., Homeier, D., Horton, A. J., Hosseinzadeh, Griffin, Hu, L., Hunkeler, J. S., Nöthe, M., Ivezić, Ž., Jain, A., Kern, N. S., Kerzendorf, W.E., Khvalko, A., King, J., Kirkby, D., Ogaz, S., Kulkarni, A. M., Sabater, J., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Oh, S., Sakurikar, P., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Parejko, J. K., Parley, N., Seifert, M., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. Xavier, Bradley, L.D., Rastogi, T., Reddy Janga, V., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Pérez-Suárez, D., Singanamalla, S., Barentsen, G., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., de Val-Borro, M., Barmby, P., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., Aldcroft, T. L., Cruz, Kelle, Baumbach, A., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Berry, K. L., Biscani, F., Boquien, Médéric, Bostroem, K. Azalee, Bouma, L.G., Brammer, G. B., Bray, E. M., Greenfield, P., Breytenbach, H., Buddelmeijer, H., Google, NumFOCUS, Space Telescope Science Institute (US), Harvard-Smithsonian Center for Astrophysics, South African Astronomical Observatory, National Aeronautics and Space Administration (US), Gordon and Betty Moore Foundation, Alfred P. Sloan Foundation, Washington Research Foundation, German Research Foundation, Gemini Observatory, Korea Astronomy and Space Science Institute, Ministerio de Economía y Competitividad (España), European Commission, Price-Whelan, Adrian M., Sipőcz, B. M., Günther, H.M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, Adam, VanderPlas, J. T., Burke, D. J., Calderone, G., Cano Rodríguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Copin, Y., Corrales, L., Groener, A. M., Crichton, D., Jenness, T., D'Avella, D., Deil, C., Depagne, É., Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Grollier, F., Kanarek, G., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Hagen, A., Hirst, P., Kendrew, S., Homeier, D., Horton, A. J., Hosseinzadeh, Griffin, Hu, L., Hunkeler, J. S., Nöthe, M., Ivezić, Ž., Jain, A., Kern, N. S., Kerzendorf, W.E., Khvalko, A., King, J., Kirkby, D., Ogaz, S., Kulkarni, A. M., Sabater, J., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., McCully, C., Montagnac, S., Oh, S., Sakurikar, P., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Parejko, J. K., Parley, N., Seifert, M., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. Xavier, Bradley, L.D., Rastogi, T., Reddy Janga, V., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Pérez-Suárez, D., Singanamalla, S., Barentsen, G., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., de Val-Borro, M., Barmby, P., Terrón, V., van Kerkwijk, M. H., de la Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., Zabalza, V., Aldcroft, T. L., Cruz, Kelle, Baumbach, A., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bach, Y. P., Bachetti, M., Bakanov, A. V., Bamford, S. P., Berry, K. L., Biscani, F., Boquien, Médéric, Bostroem, K. Azalee, Bouma, L.G., Brammer, G. B., Bray, E. M., Greenfield, P., Breytenbach, H., and Buddelmeijer, H.

Abstract

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.© 2018. The American Astronomical Society.

Published
2018

31. VizieR Online Data Catalog: VIPERS Multi-Lambda Survey (Moutard+, 2016)

Author

Moutard, T., Arnouts, S., Ilbert, O., Coupon, J., Hudelot, P., Vibert, D., Comte, V., Conseil, S., Davidzon, I., Guzzo, L., Llebaria, A., Martin, C., McCracken, H.~J., Milliard, B., Morrison, G., Schiminovich, David, Treyer, M., Werbaeke, L., Laboratoire d'Astrophysique de Marseille (LAM), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
Redshifts, [INFO]Computer Science [cs], Galaxies: photometry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS, Galaxy catalogs
Abstract

International audience; no abstract

Published
2016

32. The MUSE Hubble Ultra Deep Field Survey

Author

Inami, H., primary, Bacon, R., additional, Brinchmann, J., additional, Richard, J., additional, Contini, T., additional, Conseil, S., additional, Hamer, S., additional, Akhlaghi, M., additional, Bouché, N., additional, Clément, B., additional, Desprez, G., additional, Drake, A. B., additional, Hashimoto, T., additional, Leclercq, F., additional, Maseda, M., additional, Michel-Dansac, L., additional, Paalvast, M., additional, Tresse, L., additional, Ventou, E., additional, Kollatschny, W., additional, Boogaard, L. A., additional, Finley, H., additional, Marino, R. A., additional, Schaye, J., additional, and Wisotzki, L., additional

Published
2017
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33. The MUSE Hubble Ultra Deep Field Survey

Author

Drake, A. B., primary, Garel, T., additional, Wisotzki, L., additional, Leclercq, F., additional, Hashimoto, T., additional, Richard, J., additional, Bacon, R., additional, Blaizot, J., additional, Caruana, J., additional, Conseil, S., additional, Contini, T., additional, Guiderdoni, B., additional, Herenz, E. C., additional, Inami, H., additional, Lewis, J., additional, Mahler, G., additional, Marino, R. A., additional, Pello, R., additional, Schaye, J., additional, Verhamme, A., additional, Ventou, E., additional, and Weilbacher, P. M., additional

Published
2017
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34. The VIPERS Multi-Lambda Survey

Author

Moutard, T., primary, Arnouts, S., additional, Ilbert, O., additional, Coupon, J., additional, Hudelot, P., additional, Vibert, D., additional, Comte, V., additional, Conseil, S., additional, Davidzon, I., additional, Guzzo, L., additional, Llebaria, A., additional, Martin, C., additional, McCracken, H. J., additional, Milliard, B., additional, Morrison, G., additional, Schiminovich, D., additional, Treyer, M., additional, and Van Werbaeke, L., additional

Published
2016
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35. EMphot \mdash Photometric Software with Bayesian Priors: Application to GALEX

Author

Conseil, S., Vibert, D., Amouts, S., Milliard, B., Zamojski, M., Llebaria, A., Guillaume, Marion, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Evans, I.~N. and Accomazzi, A. and Mink, D.~J. and Rots, A.~H., Surace, Christian, and Evans, I.~N. and Accomazzi, A. and Mink, D.~J. and Rots, A.~H.

Subjects
[INFO]Computer Science [cs], [INFO] Computer Science [cs], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience; no abstract

Published
2011

36. Photometry in UV astronomical images of extended sources in crowded field using deblended images in optical visible bands as Bayesian priors

Author

Bouman, Charles A., Miller, Eric L., Pollak, Ilya, Vibert, D., Zamojski, M., Conseil, S., Llebaria, A., Arnouts, S., Milliard, B., Guillaume, M., Bouman, Charles A., Miller, Eric L., Pollak, Ilya, Vibert, D., Zamojski, M., Conseil, S., Llebaria, A., Arnouts, S., Milliard, B., and Guillaume, M.

Abstract

Photometry of astrophysical sources, galaxies and stars, in crowded field images, if an old problem, is still a challenging goal, as new space survey missions are launched, releasing new data with increased sensibility, resolution and field of view. The GALEX mission, observes in two UV bands and produces deep sky images of millions of galaxies or stars mixed together. These UV observations are of lower resolution than same field observed in visible bands, and with a very faint signal, at the level of the photon noise for a substantial fraction of objects. Our purpose is to use the better known optical counterparts as prior information in a Bayesian approach to deduce the UV flux. Photometry of extended sources has been addressed several times using various techniques: background determination via sigma clipping, adaptative-aperture, point-spread-function photometry, isophotal photometry, to lists some. The Bayesian approach of using optical priors for solving the UV photometry has already been applied by our team in a previous work. Here we describe the improvement of using the extended shape inferred by deblending the high resolution optical images and not only the position of the optical sources. The resulting photometric accuracy has been tested with simulation of crowded UV fields added on top of real UV images. Finally, this helps to converge to smaller and flat residual and increase the faint source detection threshold. It thus gives the opportunity to work on 2nd order effects, like improving the knowledge of the background or point-spread function by iterating on them.

Published
2009

40. Three Dimensional Fingertip Tracking in Stereovision.

Author

Blanc-Talon, Jacques, Philips, Wilfried, Popescu, Dan, Scheunders, Paul, Conseil, S., Bourennane, S., and Martin, L.

Abstract

This paper presents a real time estimation method of the three dimensional trajectory of a fingertip. Pointing with the finger is indeed a natural gesture for Human Computer Interaction. Our approach is based on stereoscopic vision, with two standard webcams. The hand is segmented with skin color detection, and the fingertip is detected by the analysis of the curvature of finger boundary. The fingertip tracking is carried out by a three dimensional Kalman filter, in order to improve the detection with a local research, centered on the prediction of the 3-D position, and to filter the trajectory to reduce the estimation error. [ABSTRACT FROM AUTHOR]

Published
2005
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41. The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

Author

The Astropy Collaboration, Price-Whelan, A. M., Sipőcz, B. M., Günther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., Vanderplas, J. T., Bradley, L. D., Pérez-Suárez, D., Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Cano Rodríguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Yannick Copin, Crichton, D., Dávella, D., Deil, C., Depagne, É, Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezić, Ž, Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., Mccully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Nöthe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Reddy Janga, V., Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terrón, V., Kerkwijk, M. H., La Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., and Zabalza, V.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The Astropy project supports and fosters the development of open-source and openly-developed Python packages that provide commonly-needed functionality to the astronomical community. A key element of the Astropy project is the core package Astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of inter-operable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy project., Minor changes to author list and title. Comments and feedback welcome through the paper source repository: https://github.com/astropy/astropy-v2.0-paper For more information about Astropy, see http://www.astropy.org/

42. Dark Galaxy Candidates at Redshift ∼3.5 Detected with MUSE

Author

C. Diener, Roland Bacon, Lorrie A. Straka, Joseph Caruana, Jarle Brinchmann, Raffaella Anna Marino, Thierry Contini, Sofia G. Gallego, Lutz Wisotzki, H. Finley, Elena Borisova, Simon J. Lilly, Joop Schaye, Martin Wendt, Floriane Leclercq, Johan Richard, Simon Conseil, Hanae Inami, Gabriele Pezzulli, Sowgat Muzahid, Sebastiano Cantalupo, C. Marcella Carollo, Anna Marino, R, Cantalupo, S, Lilly, S, Gallego, S, Straka, L, Borisova, E, Pezzulli, G, Bacon, R, Brinchmann, J, Carollo, C, Caruana, J, Conseil, S, Contini, T, Diener, C, Finley, H, Inami, H, Leclercq, F, Muzahid, S, Richard, J, Schaye, J, Wendt, M, Wisotzki, L, Department of Computer Science [ETH Zürich] (D-INFK), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010305 fluids & plasmas, Red shift -- Observations, galaxies: high-redshift, quasars: general, 0103 physical sciences, Galaxy formation and evolution, galaxies: formation, Cosmology -- Observations, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Galaxies -- Observations, Galaxies -- Formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, Astronomy and Astrophysics, Quasar, Galaxies, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Cosmology, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxies -- Evolution, galaxies: star formation, Dark galaxy, intergalactic medium, Equivalent width, quasars: emission line
Abstract

Recent theoretical models suggest that the early phase of galaxy formation could involve an epoch when galaxies are gas-rich but inefficient at forming stars: a "dark galaxy" phase. Here, we report the results of our MUSE (Multi Unit Spectroscopic Explorer) survey for dark galaxies fluorescently illuminated by quasars at $z>3$. Compared to previous studies which are based on deep narrow-band (NB) imaging, our integral field survey provides a nearly uniform sensitivity coverage over a large volume in redshift space around the quasars as well as full spectral information at each location. Thanks to these unique features, we are able to build control samples at large redshift distances from the quasars using the same data taken under the same conditions. By comparing the rest-frame equivalent width (EW$_{0}$) distributions of the Ly$\alpha$ sources detected in proximity to the quasars and in control samples, we detect a clear correlation between the locations of high EW$_{0}$ objects and the quasars. This correlation is not seen in other properties such as Ly$\alpha$ luminosities or volume overdensities, suggesting the possible fluorescent nature of at least some of these objects. Among these, we find 6 sources without continuum counterparts and EW$_{0}$ limits larger than $240\,\mathrm{\AA}$ that are the best candidates for dark galaxies in our survey at $z>3.5$. The volume densities and properties, including inferred gas masses and star formation efficiencies, of these dark galaxy candidates are similar to previously detected candidates at $z\approx2.4$ in NB surveys. Moreover, if the most distant of these are fluorescently illuminated by the quasar, our results also provide a lower limit of $t=60$ Myr on the quasar lifetime., Comment: 28 pages, 13 figures, 5 tables, submitted to ApJ

Published
2018
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43. The MUSE Hubble Ultra Deep Field Survey

Author

Jeremy Blaizot, Mohammad Akhlaghi, Peter D. Mitchell, Hanae Inami, Simon Conseil, Roland Bacon, Sebastiano Cantalupo, Marcella Carollo, Floriane Leclercq, Johan Richard, Anne Verhamme, Joop Schaye, Jarle Brinchmann, Raffaella Anna Marino, Michael V. Maseda, Thierry Contini, Edmund Christian Herenz, Lutz Wisotzki, Takuya Hashimoto, Thibault Garel, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Chimie de Strasbourg, Université de Strasbourg (UNISTRA)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Leclercq, F, Bacon, R, Wisotzki, L, Mitchell, P, Garel, T, Verhamme, A, Blaizot, J, Hashimoto, T, Herenz, E, Conseil, S, Cantalupo, S, Inami, H, Contini, T, Richard, J, Maseda, M, Schaye, J, Marino, R, Akhlaghi, M, Brinchmann, J, Carollo, M, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)

Subjects
Physics, 010308 nuclear & particles physics, Continuum (design consultancy), Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Hubble Ultra-Deep Field, 01 natural sciences, Cosmology: observation, Galaxy, Redshift, Accretion (astrophysics), Dark matter halo, 13. Climate action, Space and Planetary Science, galaxies: high-redshift, cosmology: observations, 0103 physical sciences, Satellite galaxy, galaxies: formation, Halo, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report the detection of extended Lyα haloes around 145 individual star-forming galaxies at redshifts 3 ≤ z ≤ 6 in the Hubble Ultra Deep Field observed with the Multi-Unit Spectroscopic Explorer (MUSE) at ESO-VLT. Our sample consists of continuum-faint (− 15 ≥ MUV ≥ −22) Lyα emitters (LAEs). Using a 2D, two-component (continuum-like and halo) decomposition of Lyα emission assuming circular exponential distributions, we measure scale lengths and luminosities of Lyα haloes. We find that 80% of our objects having reliable Lyα halo measurements show Lyα emission that is significantly more extended than the UV continuum detected by HST (by a factor ≈4 to >20). The median exponential scale length of the Lyα haloes in our sample is ≈4.5 kpc with a few haloes exceeding 10 kpc. By comparing the maximal detected extent of the Lyα emission with the predicted dark matter halo virial radii of simulated galaxies, we show that the detected Lyα emission of our selected sample of Lyα emitters probes a significant portion of the cold circum-galactic medium of these galaxies (>50% in average). This result therefore shows that there must be significant HI reservoirs in the circum-galactic medium and reinforces the idea that Lyα haloes are ubiquitous around high-redshift Lyα emitting galaxies. Our characterization of the Lyα haloes indicates that the majority of the Lyα flux comes from the halo (≈65%) and that their scale lengths seem to be linked to the UV properties of the galaxies (sizes and magnitudes). We do not observe a significant Lyα halo size evolution with redshift, although our sample for z> 5 is very small. We also explore the diversity of the Lyα line profiles in our sample and we find that the Lyα lines cover a large range of full width at half maximum (FWHM) from 118 to 512 km s-1. While the FWHM does not seem to be correlated to the Lyα scale length, most compact Lyα haloes and those that are not detected with high significance tend to have narrower Lyα profiles (-1). Finally, we investigate the origin of the extended Lyα emission but we conclude that our data do not allow us to disentangle the possible processes, i.e. scattering from star-forming regions, fluorescence, cooling radiation from cold gas accretion, and emission from satellite galaxies.

Published
2017
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44. The MUSE Hubble Ultra Deep Field Survey : XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3

Author

Raffaella Anna Marino, Gabriele Pezzulli, Thibault Garel, Edmund Christian Herenz, Jérémy Blaizot, Sebastiano Cantalupo, Floriane Leclercq, Anne Verhamme, Lutz Wisotzki, Adélaïde Claeyssens, Kasper B. Schmidt, Haruka Kusakabe, Takuya Hashimoto, Simon Conseil, Peter D. Mitchell, Jorryt Matthee, Michael V. Maseda, Johan Richard, Roland Bacon, Jarle Brinchmann, Thierry Contini, Leclercq, F, Bacon, R, Verhamme, A, Garel, T, Blaizot, J, Brinchmann, J, Cantalupo, S, Claeyssens, A, Conseil, S, Contini, T, Hashimoto, T, Herenz, E, Kusakabe, H, Marino, R, Maseda, M, Matthee, J, Mitchell, P, Pezzuli, G, Richard, J, Schmidt, K, Wisotzki, L, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Scattering, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, Hubble Ultra-Deep Field, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Cosmology: observation, Redshift, Galaxy, Full width at half maximum, Wavelength, Space and Planetary Science, 0103 physical sciences, Radiative transfer, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present spatially resolved maps of six individually-detected Lyman alpha haloes (LAHs) as well as a first statistical analysis of the Lyman alpha (Lya) spectral signature in the circum-galactic medium of high-redshift star-forming galaxies using MUSE. Our resolved spectroscopic analysis of the LAHs reveals significant intrahalo variations of the Lya line profile. Using a three-dimensional two-component model for the Lya emission, we measure the full width at half maximum (FWHM), the peak velocity shift and the asymmetry of the Lya line in the core and in the halo of 19 galaxies. We find that the Lya line shape is statistically different in the halo compared to the core for ~40% of our galaxies. Similarly to object-by-object based studies and a recent resolved study using lensing, we find a correlation between the peak velocity shift and the width of the Lya line both at the interstellar and circum-galactic scales. While there is a lack of correlation between the spectral properties and the spatial scale lengths of our LAHs, we find a correlation between the width of the line in the LAH and the halo flux fraction. Interestingly, UV bright galaxies show broader, more redshifted and less asymmetric Lya lines in their haloes. The most significant correlation found is for the FWHM of the line and the UV continuum slope of the galaxy, suggesting that the redder galaxies have broader Lya lines. The generally broad and red line shapes found in the halo component suggests that the Lya haloes are powered either by scattering processes through an outflowing medium, fluorescent emission from outflowing cold clumps of gas, or a mix of both. Considering the large diversity of the Lya line profiles observed in our sample and the lack of strong correlation, the interpretation of our results is still broadly open and underlines the need for realistic spatially resolved models of the LAHs., Comment: 17+4 pages, 12+3 figures, 2+1 tables, accepted for publication in A&A

Published
2020
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