학술논문
Euclid preparation. The Near-IR Background Dipole Experiment with Euclid
Document Type
Working Paper
Author
Euclid Collaboration; Kashlinsky, A.; Arendt, R. G.; Ashby, M. L. N.; Atrio-Barandela, F.; Scaramella, R.; Strauss, M. A.; Altieri, B.; Amara, A.; Andreon, S.; Auricchio, N.; Baldi, M.; Bardelli, S.; Bender, R.; Bodendorf, C.; Branchini, E.; Brescia, M.; Brinchmann, J.; Camera, S.; Capobianco, V.; Carbone, C.; Carretero, J.; Casas, S.; Castellano, M.; Cavuoti, S.; Cimatti, A.; Congedo, G.; Conselice, C. J.; Conversi, L.; Copin, Y.; Corcione, L.; Courbin, F.; Courtois, H. M.; Da Silva, A.; Degaudenzi, H.; Di Giorgio, A. M.; Dinis, J.; Dubath, F.; Dupac, X.; Dusini, S.; Ealet, A.; Farina, M.; Farrens, S.; Ferriol, S.; Frailis, M.; Franceschi, E.; Galeotta, S.; Gillis, B.; Giocoli, C.; Grazian, A.; Grupp, F.; Haugan, S. V. H.; Hook, I.; Hormuth, F.; Hornstrup, A.; Jahnke, K.; Keihänen, E.; Kermiche, S.; Kiessling, A.; Kilbinger, M.; Kubik, B.; Kunz, M.; Kurki-Suonio, H.; Ligori, S.; Lilje, P. B.; Lindholm, V.; Lloro, I.; Maino, D.; Maiorano, E.; Mansutti, O.; Marggraf, O.; Markovic, K.; Martinet, N.; Marulli, F.; Massey, R.; Maurogordato, S.; McCracken, H. J.; Medinaceli, E.; Mei, S.; Mellier, Y.; Meneghetti, M.; Meylan, G.; Moresco, M.; Moscardini, L.; Munari, E.; Niemi, S. -M.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.; Percival, W. J.; Pires, S.; Polenta, G.; Poncet, M.; Popa, L. A.; Raison, F.; Renzi, A.; Rhodes, J.; Riccio, G.; Romelli, E.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Sapone, D.; Sartoris, B.; Schirmer, M.; Schneider, P.; Schrabback, T.; Secroun, A.; Seidel, G.; Seiffert, M.; Serrano, S.; Sirignano, C.; Sirri, G.; Stanco, L.; Surace, C.; Tallada-Crespí, P.; Taylor, A. N.; Teplitz, H. I.; Tereno, I.; Toledo-Moreo, R.; Torradeflot, F.; Tutusaus, I.; Valenziano, L.; Vassallo, T.; Veropalumbo, A.; Wang, Y.; Zamorani, G.; Zoubian, J.; Zucca, E.; Biviano, A.; Bozzo, E.; Burigana, C.; Colodro-Conde, C.; Di Ferdinando, D.; Fabbian, G.; Farinelli, R.; Graciá-Carpio, J.; Mainetti, G.; Martinelli, M.; Mauri, N.; Neissner, C.; Sakr, Z.; Scottez, V.; Tenti, M.; Viel, M.; Wiesmann, M.; Akrami, Y.; Allevato, V.; Anselmi, S.; Baccigalupi, C.; Ballardini, M.; Blanchard, A.; Borgani, S.; Borlaff, A. S.; Bruton, S.; Cabanac, R.; Cappi, A.; Carvalho, C. S.; Castignani, G.; Castro, T.; {n}as-Herrera, G. Ca\; Chambers, K. C.; Contarini, S.; Coupon, J.; De Lucia, G.; Desprez, G.; Di Domizio, S.; Dole, H.; Díaz-Sánchez, A.; Vigo, J. A. Escartin; Ferrero, I.; Finelli, F.; Gabarra, L.; García-Bellido, J.; Gautard, V.; Gaztanaga, E.; George, K.; Giacomini, F.; Gozaliasl, G.; Gregorio, A.; Hall, A.; Hildebrandt, H.; Kajava, J. J. E.; Kansal, V.; Kirkpatrick, C. C.; Legrand, L.; Loureiro, A.; Magliocchetti, M.; Mannucci, F.; Maoli, R.; Martins, C. J. A. P.; Matthew, S.; Maurin, L.; Metcalf, R. B.; Migliaccio, M.; Monaco, P.; Morgante, G.; Nadathur, S.; Walton, Nicholas A.; Patrizii, L.; Popa, V.; Potter, D.; Pöntinen, M.; Rocci, P. -F.; Sahlén, M.; Schneider, A.; Sefusatti, E.; Sereno, M.; Steinwagner, J.; Testera, G.; Teyssier, R.; Toft, S.; Tosi, S.; Troja, A.; Tucci, M.; Valiviita, J.; Vergani, D.; Verza, G.; Hasinger, G.
Source
Subject
Language
Abstract
Verifying the fully kinematic nature of the cosmic microwave background (CMB) dipole is of fundamental importance in cosmology. In the standard cosmological model with the Friedman-Lemaitre-Robertson-Walker (FLRW) metric from the inflationary expansion the CMB dipole should be entirely kinematic. Any non-kinematic CMB dipole component would thus reflect the preinflationary structure of spacetime probing the extent of the FLRW applicability. Cosmic backgrounds from galaxies after the matter-radiation decoupling, should have kinematic dipole component identical in velocity with the CMB kinematic dipole. Comparing the two can lead to isolating the CMB non-kinematic dipole. It was recently proposed that such measurement can be done using the near-IR cosmic infrared background (CIB) measured with the currently operating Euclid telescope, and later with Roman. The proposed method reconstructs the resolved CIB, the Integrated Galaxy Light (IGL), from Euclid's Wide Survey and probes its dipole, with a kinematic component amplified over that of the CMB by the Compton-Getting effect. The amplification coupled with the extensive galaxy samples forming the IGL would determine the CIB dipole with an overwhelming signal/noise, isolating its direction to sub-degree accuracy. We develop details of the method for Euclid's Wide Survey in 4 bands spanning 0.6 to 2 mic. We isolate the systematic and other uncertainties and present methodologies to minimize them, after confining the sample to the magnitude range with negligible IGL/CIB dipole from galaxy clustering. These include the required star-galaxy separation, accounting for the extinction correction dipole using the method newly developed here achieving total separation, accounting for the Earth's orbital motion and other systematic effects. (Abridged)
Comment: Euclid Key Project paper, A&A submitted
Comment: Euclid Key Project paper, A&A submitted