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1. Prompt Detection of Fast Optical Bursts with the Vera C. Rubin Observatory

Author

Homar, Guillem Megias, Meyers, Joshua E., and Kahn, Steven M.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The transient optical sky has remained largely unexplored on very short timescales. While there have been some experiments searching for optical transients from minutes to years, none have had the capability to distinguish millisecond Fast Optical Bursts (FOB). Such very fast transients could be the optical counterparts of Fast Radio Bursts (FRB), the prompt emission from $\gamma$-Ray Bursts (GRB), or other previously unknown phenomena. Here, we investigate a novel approach to the serendipitous detection of FOBs, which relies on searching for anomalous spatial images. In particular, due to their short duration, the seeing distorted images of FOBs should look characteristically different than those of steady sources in a standard optical exposure of finite duration. We apply this idea to simulated observations with the Vera C. Rubin Observatory, produced by tracing individual photons through a turbulent atmosphere, and down through the optics and camera of the Rubin telescope. We compare these simulated images to steady-source star simulations in 15 s integrations, the nominal Rubin exposure time. We report the classification accuracy results of a Neural Network classifier for distinguishing FOBs from steady sources. From this classifier, we derive constraints in duration-intensity parameter space for unambiguously identifying FOBs in Rubin observations. We conclude with estimates of the total number of detections of FOB counterparts to FRBs expected during the 10-year Rubin Legacy Survey of Space and Time (LSST)., Comment: 7 pages, 4 figures, submitted to the Astrophysical Journal

Published
2023
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2. Snowmass2021 Cosmic Frontier White Paper: Rubin Observatory after LSST

Author

Blum, Bob, Digel, Seth W., Drlica-Wagner, Alex, Habib, Salman, Heitmann, Katrin, Ishak, Mustapha, Jha, Saurabh W., Kahn, Steven M., Mandelbaum, Rachel, Marshall, Phil, Newman, Jeffrey A., Roodman, Aaron, and Stubbs, Christopher W.

Subjects
High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Vera C. Rubin Observatory will begin the Legacy Survey of Space and Time (LSST) in 2024, spanning an area of 18,000 square degrees in six bands, with more than 800 observations of each field over ten years. The unprecedented data set will enable great advances in the study of the formation and evolution of structure and exploration of physics of the dark universe. The observations will hold clues about the cause for the accelerated expansion of the universe and possibly the nature of dark matter. During the next decade, LSST will be able to confirm or dispute if tensions seen today in cosmological data are due to new physics. New and unexpected phenomena could confirm or disrupt our current understanding of the universe. Findings from LSST will guide the path forward post-LSST. The Rubin Observatory will still be a uniquely powerful facility even then, capable of revealing further insights into the physics of the dark universe. These could be obtained via innovative observing strategies, e.g., targeting new probes at shorter timescales than with LSST, or via modest instrumental changes, e.g., new filters, or through an entirely new instrument for the focal plane. This White Paper highlights some of the opportunities in each scenario from Rubin observations after LSST., Comment: Contribution to Snowmass 2021

Published
2022
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3. LSST: From Science Drivers to Reference Design and Anticipated Data Products

Author

Ivezić, Željko, Kahn, Steven M, Tyson, J Anthony, Abel, Bob, Acosta, Emily, Allsman, Robyn, Alonso, David, AlSayyad, Yusra, Anderson, Scott F, Andrew, John, Angel, James Roger P, Angeli, George Z, Ansari, Reza, Antilogus, Pierre, Araujo, Constanza, Armstrong, Robert, Arndt, Kirk T, Astier, Pierre, Aubourg, Éric, Auza, Nicole, Axelrod, Tim S, Bard, Deborah J, Barr, Jeff D, Barrau, Aurelian, Bartlett, James G, Bauer, Amanda E, Bauman, Brian J, Baumont, Sylvain, Bechtol, Ellen, Bechtol, Keith, Becker, Andrew C, Becla, Jacek, Beldica, Cristina, Bellavia, Steve, Bianco, Federica B, Biswas, Rahul, Blanc, Guillaume, Blazek, Jonathan, Blandford, Roger D, Bloom, Josh S, Bogart, Joanne, Bond, Tim W, Booth, Michael T, Borgland, Anders W, Borne, Kirk, Bosch, James F, Boutigny, Dominique, Brackett, Craig A, Bradshaw, Andrew, Brandt, William Nielsen, Brown, Michael E, Bullock, James S, Burchat, Patricia, Burke, David L, Cagnoli, Gianpietro, Calabrese, Daniel, Callahan, Shawn, Callen, Alice L, Carlin, Jeffrey L, Carlson, Erin L, Chandrasekharan, Srinivasan, Charles-Emerson, Glenaver, Chesley, Steve, Cheu, Elliott C, Chiang, Hsin-Fang, Chiang, James, Chirino, Carol, Chow, Derek, Ciardi, David R, Claver, Charles F, Cohen-Tanugi, Johann, Cockrum, Joseph J, Coles, Rebecca, Connolly, Andrew J, Cook, Kem H, Cooray, Asantha, Covey, Kevin R, Cribbs, Chris, Cui, Wei, Cutri, Roc, Daly, Philip N, Daniel, Scott F, Daruich, Felipe, Daubard, Guillaume, Daues, Greg, Dawson, William, Delgado, Francisco, Dellapenna, Alfred, de Peyster, Robert, de Val-Borro, Miguel, Digel, Seth W, Doherty, Peter, Dubois, Richard, Dubois-Felsmann, Gregory P, Durech, Josef, Economou, Frossie, Eifler, Tim, Eracleous, Michael, Emmons, Benjamin L, and Neto, Angelo Fausti

Subjects
general [stars], Organic Chemistry, observational [methods], Molecular, Astronomy & Astrophysics, Physical Chemistry, Atomic, observations [cosmology], Particle and Plasma Physics, surveys, astro-ph, astrometry, Nuclear, general [Galaxy], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the solar system, exploring the transient optical sky, and mapping the Milky Way. LSST will be a large, wide-field ground-based system designed to obtain repeated images covering the sky visible from Cerro Pachón in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg 2 field of view, a 3.2-gigapixel camera, and six filters (ugrizy) covering the wavelength range 320-1050 nm. The project is in the construction phase and will begin regular survey operations by 2022. About 90% of the observing time will be devoted to a deep-wide-fast survey mode that will uniformly observe a 18,000 deg 2 region about 800 times (summed over all six bands) during the anticipated 10 yr of operations and will yield a co-added map to r ∼27.5. These data will result in databases including about 32 trillion observations of 20 billion galaxies and a similar number of stars, and they will serve the majority of the primary science programs. The remaining 10% of the observing time will be allocated to special projects such as Very Deep and Very Fast time domain surveys, whose details are currently under discussion. We illustrate how the LSST science drivers led to these choices of system parameters, and we describe the expected data products and their characteristics.

Published
2019

4. On the Putative Detection of z>0 X-ray Absorption Features in the Spectrum of Markarian 421

Author

Rasmussen, Andrew P., Kahn, Steven M., Paerels, Frits, Herder, Jan Willem den, Kaastra, Jelle, and de Vries, Cor

Subjects
Astrophysics (astro-ph), FOS: Physical sciences
Abstract

In a series of papers, Nicastro et al. have reported the detection of z>0 OVII absorption features in the spectrum of Mrk421 obtained with the Chandra Low Energy Transmission Grating Spectrometer (LETGS). We evaluate this result in the context of a high quality spectrum of the same source obtained with the Reflection Grating Spectrometer (RGS) on XMM-Newton. The data comprise over 955ks of usable exposure time and more than 26000 counts per 50 milliAngstrom at 21.6 Angstroms. We concentrate on the spectrally clean region (21.3 < lambda < 22.5 Angstroms) where sharp features due to the astrophysically abundant OVII may reveal an intervening, warm--hot intergalactic medium (WHIM). We do not confirm detection of any of the intervening systems claimed to date. Rather, we detect only three unsurprising, astrophysically expected features down to the Log(N_i)~14.6 (3 sigma) sensitivity level. Each of the two purported WHIM features is rejected with a statistical confidence that exceeds that reported for its initial detection. While we can not rule out the existence of fainter, WHIM related features in these spectra, we suggest that previous discovery claims were premature. A more recent paper by Williams et al. claims to have demonstrated that the RGS data we analyze here do not have the resolution or statistical quality required to confirm or deny the LETGS detections. We show that our careful analysis resolves the issues encountered by Williams et al. and recovers the full resolution and statistical quality of the RGS data. We highlight the differences between our analysis and those published by Williams et al. as this may explain our disparate conclusions., 19 pages/7 figures/4 tables. 060424 submitted to ApJ 060522 re-submitted following ApJ request

Published
2006
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5. Evidence for the importance of resonance scattering in X-ray emission line profiles of the O star $��$ Puppis

Author

Leutenegger, Maurice A., Owocki, Stanley P., Kahn, Steven M., and Paerels, Frits B. S.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences
Abstract

We fit the Doppler profiles of the He-like triplet complexes of \ion{O}{7} and \ion{N}{6} in the X-ray spectrum of the O star $��$ Puppis, using XMM-Newton RGS data collected over $\sim 400$ ks of exposure. We find that they cannot be well fit if the resonance and intercombination lines are constrained to have the same profile shape. However, a significantly better fit is achieved with a model incorporating the effects of resonance scattering, which causes the resonance line to become more symmetric than the intercombination line for a given characteristic continuum optical depth $��_*$. We discuss the plausibility of this hypothesis, as well as its significance for our understanding of Doppler profiles of X-ray emission lines in O stars., 29 pages, 8 figures, revised version accepted by ApJ

Published
2006
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6. Resolving the Effects of Resonant X-ray Line Scattering in Cen X-3 with Chandra

Author

Wojdowski, Patrick S., Liedahl, Duane A., Sako, Masao, Kahn, Steven M., and Paerels, Frederik

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics
Abstract

The massive X-ray binary Cen X-3 was observed over approximately one quarter of the system's 2.08 day orbit, beginning before eclipse and ending slightly after eclipse center with the Chandra X-ray Observatory using its High-Energy Transmission Grating Spectrometer. The spectra show K shell emission lines from hydrogen- and helium-like ions of magnesium, silicon, sulfur, and iron as well as a K-alpha fluorescence emission feature from near-neutral iron. The helium-like n=2->1 triplet of silicon is fully resolved and the analogous triplet of iron is partially resolved. The helium-like triplet component flux ratios outside of eclipse are consistent with emission from recombination and subsequent cascades (recombination radiation) from a photoionized plasma. In eclipse, however, the w (resonance) lines of silicon and iron are stronger than that expected for recombination radiation, and are consistent with emission from a collisionally ionized plasma. The triplet line flux ratios at both phases can be explained more naturally, however, as emission from a photoionized plasma if the effects of resonant line scattering are included in addition to recombination radiation. We show that the emissivity due to resonant scattering depends sensitively on the line optical depth and, in the case of winds in X-ray binaries, this allows constraints on the wind velocity even when Doppler shifts cannot be resolved., 31 pages, 8 figures, ApJ accepted, abridged in accord with referee's Comments

Published
2002
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7. Soft X-ray Spectra of Seyfert 2 Galaxies

Author

Sako, Masao, Kinkhabwala, Ali, Kahn, Steven M., Behar, Ehud, Paerels, Frits, Gu, Ming Feng, Brinkman, Albert C., Kaastra, Jelle S., and Liedahl, Duane A.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

High resolution spectroscopic observations of Seyfert galaxies with Chandra and XMM-Newton allows us to study the detailed ionization and thermal structures of the X-ray absorbing/emitting material in the circumnuclear environment. The vast improvement in the spectral resolving power by more than an order of magnitude enables us, for the first time, to unambiguously distinguish the dominant line emission mechanisms and to measure its dynamical properties as well. The X-ray band harbors spectral transitions from a wide range of ionization states, including valence-shell transitions in K-shell and L-shell ions from most cosmically abundant elements, as well as inner-shell transitions of iron and other mid-Z elements, which can be probed through absorption measurements. The X-ray spectrum, therefore, provides simultaneous velocity and column density constraints of highly ionized to only slightly ionized gas harbored in many of these systems. We summarize recent results that have emerged from observations of Seyfert 2 galaxies with the grating spectrometers onboard Chandra and XMM-Newton. We give particular emphasis to an empirical physical model that we have developed based on the observed spectra, and how it can be used for comparative studies with Seyfert 1 galaxies to test the AGN unification scenarios., Comment: 8 pages, 7 figures. Invited review. To appear in the proceedings of the workshop "X-ray spectroscopy of AGN with Chandra and XMM-Newton", eds., Th. Boller, S. Komossa, S. Kahn, and H. Kunieda

Published
2002
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8. X-ray spectroscopy of Eta Carinae with XMM-Newton

Author

Leutenegger, Maurice A., Kahn, Steven M., and Ramsay, Gavin

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

We present XMM-Newton observations of the luminous star Eta Carinae, including a high resolution soft X-ray spectrum of the surrounding nebula obtained with the Reflection Grating Spectrometer. The EPIC image of the field around Eta Car shows many early-type stars and diffuse emission from hot, shocked gas. The EPIC spectrum of the star is similar to that observed in previous X-ray observations, and requires two temperature components. The RGS spectrum of the surrounding nebula shows K-shell emission lines from hydrogen- and helium-like nitrogen and neon and L-shell lines from iron, but little or no emission from oxygen. The observed emission lines are not consistent with a single temperature, but the range of temperatures observed is not large, spanning ~0.15-0.6 keV. We obtain upper limits for oxygen line emission and derive a lower limit of N/O > 9. This is consistent with previous abundance determinations for the ejecta of Eta Car, and with theoretical models for the evolution of massive, rotating stars., 20 pages, 8 figures, accepted by ApJ

Published
2002
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10. The X-ray observatory Suzaku

Author

Bautz, Mark, Kelley, Richard L., Petre, Robert, Figueroa, Enectali, Soong, Yang, Gendreau, Keith, Griffiths, Richard E., Harrus, Ilana, White, Nicholas E., Hasinger, Gunther, Henry, Patrick J., Holt, Stephen S., Hornschemeier, Ann, Hughes, John P., Hwang, Una, Smith, Randall, Kahn, Steven M., Kilbourne, Caroline, Kissel, Steve, Szymkowiak, Andrew E., Madejski, Greg M., Markowitz, Alex, Matsumoto, Chiho, Matsumoto, Hironori, Mccammon, Dan, Moseley, Harvey, Mushotzky, Richard, Nousek, John A., Chan, Kai-Wing, Ozawa, Hideki, Parmer, Arvind N., Pence, William D., Turner, Martin J. L., Angelini, Lorella, Arnaud, Keith, Boyce, Kevin, Brown, Gregory V., Porter, F. Scott, Cottam, Jean, Reeves, James N., Ricker, George R., Doty, John, Sanders, Wilton T., Fabian, Andrew C., Serlemitsos, Peter, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tomida, Hiroshi, Torii, Ken'ichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsuru, Takeshi Go, Ueda, Yoshihiro, Ueno, Shiro, Ueno, Masaru, Uno, Shin'ichiro, Urata, Yuji, Watanabe, Shin, Yamamoto, Norimasa, Ishida, Manabu, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Ishisaki, Yoshitaka, Isobe, Naoki, Itoh, Masayuki, Iyomoto, Naoko, Kamae, Tuneyoshi, Katagiri, Hideaki, Kataoka, Jun, Mitsuda, Kazuhisa, Inoue, Hajime, Katayama, Haruyoshi, Koyama, Katsuji, Kunieda, Hideyo, Makishima, Kazuo, Ogawara, Yoshiaki, Takahashi, Tadayuki, Tsunemi, Hiroshi, Anabuki, Naohisa, Kawai, Nobuyuki, Awaki, Hisamitsu, Bamba, Aya, Dotani, Tadayasu, Ebisawa, Ken, Ezoe, Yuichiro, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furusho, Tae, Furuzawa, Akihiro, Kinugasa, Kenzo, Haba, Yoshito, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashida, Kiyoshi, Hiraga, Junko S., Kitamoto, Shunji, Kohama, Mitsuhiro, Kohmura, Takayoshi, Kokubun, Motohide, Kotani, Taro, Kotoku, Jun'ichi, Kubota, Aya, Maeda, Yoshitomo, Makino, Fumiyoshi, Matsuoka, Masaru, Matsushita, Kyoko, Mihara, Tatehiko, Misaki, Kazutami, Miyata, Emi, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Morii, Mikio, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Nagase, Fumiaki, Namiki, Masaaki, Negoro, Hitoshi, Nakazawa, Kazuhiro, Okajima, Takashi, Ogasaka, Yasushi, Ohashi, Takaya, Oshima, Tai, Ota, Naomi, Ozaki, Masanobu, Sakurai, Ikuya, Senda, Atsushi, Shibata, Ryo, Suzuki, Motoko, Takahashi, Hiromitsu, Tamagawa, Toru, Tamura, Keisuke, Tamura, Takayuki, and Tanaka, Yasuo

Subjects
Physics, Scientific instrument, instrumentation, Spacecraft, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics, X-rays: general, Space and Planetary Science, Observatory, space vehicles, space vehicles: instruments, business
Abstract

著者人数: 143名, Accepted: 2006-09-27, 資料番号: SA1000631000

11. Large Synoptic Survey Telescope: Dark Energy Science Collaboration

Author

Abate, Alexandra, Aldering, Greg, Allen, Steven W., Ansari, Reza, Antilogus, Pierre, Applegate, Douglas, Astier, Pierre, Aubourg, Eric, Bahcall, Neta A., Bard, Deborah, Barkhouse, Wayne A., Bartlett, James G., Bean, Rachel, Becker, Andrew, Beckmann, Volcker, Bernstein, Gary, Biswas, Rahul, Blanc, Guillaume, Bongard, Sebastien, Bosch, James, Boutigny, Dominique, Bradac, Marusa, Bradshaw, Andrew, Brunner, Robert J., Burchat, Patricia R., Burke, David L., Cahn, Robert, Campagne, Jean-Eric, Carrasco Kind, Matias, Chihway Chang, Cheu, Elliott C., Chiang, James, Cinabro, David, Claver, Chuck, Clowe, Douglas, Cohn, Joanne D., Connolly, Andrew, Cooray, Asantha, Croft, Rupert A. C., Cui, Wei, Cunha, Carlos, Antonio, Ian P., Digel, Seth W., Di Matteo, Tiziana, Dodelson, Scott, Dore, Olivier, Dubois, Richard, Dubois-Felsmann, Gregory P., Ealet, Anne, Escoffier, Stephanie, Fassnacht, Chris, Finley, David A., Fouchez, Dominique, Frieman, Joshua A., Ganga, Ken, Gangler, Emmanuel, Garzoglio, Gabriele, Gawiser, Eric, Gilman, Fred, Gilmore, Kirk, Gladney, Larry, Glanzman, Thomas, Gottschalk, Erik E., Gnedin, Nickolay Y., Gris, Philippe, Guy, Julien, Habib, Salman, Heitmann, Katrin, Hilbert, Stefan, Ho, Shirley, Hogan, Craig, Honscheid, Klaus, Huard, Zachary, Huff, Eric M., Ivezic, Zeljko, Jain, Bhuvnesh, Jarvis, Mike, Jee, M. James, Jeltema, Tesla, Jha, Saurabh W., Johns, Kenneth A., Johnson, Anthony S., Johnson, Robert P., Kahn, Steven M., Kent, Stephen, Kessler, Richard, Kiessling, Alina, Kim, Alex G., Kirkby, David, Kirshner, Robert P., Kovacs, Eve V., Knox, Lloyd, Kratochvil, Jan M., Kuhlmann, Steve, Levi, Michael, Li, Guoliang, Lin, Huan, Linder, Eric, Lupton, Robert, Ma, Zhaoming, Macintosh, Bruce, Mandelbaum, Rachel, Mantz, Adam, Marshall, Philip J., Marshall, Stuart, May, Morgan, Mcdonald, Patrick, Meadows, Brian, Melchior, Peter M., Menard, Brice, Moniez, Marc, Morandi, Andrea, Morris, R. Glenn, Newman, Jeffrey A., Neyrinck, Mark C., Nugent, Peter, O Connor, Paul, Olivier, Scot S., Padmanabhan, Nikhil, Pain, Reynald, Peng, En-Hsin, Perdereau, Olivier, Perlmutter, Saul, Peterson, John R., Petrosian, Vahé, Plaszczynski, Stephane, Pope, Adrian C., Raccanelli, Alvise, Rasmussen, Andrew, Reil, Kevin, Rhodes, Jason, Ricker, Paul M., Ricol, Jean-Stephane, Roe, Natalie, Roodman, Aaron, Rosenberg, Leslie, Roucelle, Cecile, Russo, Stefano, Sako, Masao, Schindler, Rafe H., Schmidt, Samuel J., Schneider, Michael D., Sehgal, Neelima, Seljak, Uros, Sembroski, Glenn, Seo, Hee-Jong, Shipsey, Ian, Singal, Jack, Spergel, David, Soares-Santos, Marcelle, Spinka, Harold, Stebbins, Albert, Strauss, Michael A., Stubbs, Christopher W., Tao, Charling, Thaler, Jon J., Thomas, Rollin C., Thorman, Paul A., Tilquin, Andre, Trac, Hy, Treu, Tommaso, Tristram, Matthieu, Tyson, J. Anthony, Wandelt, Benjamin D., Wang, Yun, Wechsler, Risa H., Wenaus, Torre, White, Martin, Wittman, David, Wood-Vasey, W. Michael, Xin, Bo, Yoachim, Peter, Zentner, Andrew R., and Zhan, Hu

12. LSST Science Book, Version 2.0

Author

Lsst, Science Collaboration, Abell, Paul A., Allison, Julius, Anderson, Scott F., Andrew, John R., Angel, J. Roger P., Armus, Lee, Arnett, David, Asztalos, S. J., Axelrod, Tim S., Bailey, Stephen, Ballantyne, D. R., Bankert, Justin R., Barkhouse, Wayne A., Barr, Jeffrey D., Barrientos, L. Felipe, Barth, Aaron J., Bartlett, James G., Becker, Andrew C., Becla, Jacek, Beers, Timothy C., Bernstein, Joseph P., Biswas, Rahul, Blanton, Michael R., Bloom, Joshua S., Bochanski, John J., Boeshaar, Pat, Borne, Kirk D., Bradac, Marusa, Brandt, W. N., Bridge, Carrie R., Brown, Michael E., Brunner, Robert J., Bullock, James S., Burgasser, Adam J., Burge, James H., Burke, David L., Cargile, Phillip A., Chandrasekharan, Srinivasan, Chartas, George, Chesley, Steven R., Chu, You-Hua, Cinabro, David, Claire, Mark W., Claver, Charles F., Clowe, Douglas, Connolly, A. J., Cook, Kem H., Cooke, Jeff, Cooray, Asantha, Covey, Kevin R., Culliton, Christopher S., Jong, Roelof, Vries, Willem H., Debattista, Victor P., Delgado, Francisco, Antonio, Ian P., Dhital, Saurav, Di Stefano, Rosanne, Dickinson, Mark, Dilday, Benjamin, Djorgovski, S. G., Dobler, Gregory, Donalek, Ciro, Dubois-Felsmann, Gregory, Durech, Josef, Eliasdottir, Ardis, Eracleous, Michael, Eyer, Laurent, Falco, Emilio E., Fan, Xiaohui, Fassnacht, Christopher D., Ferguson, Harry C., Fernandez, Yanga R., Fields, Brian D., Finkbeiner, Douglas, Figueroa, Eduardo E., Fox, Derek B., Francke, Harold, Frank, James S., Frieman, Josh, Fromenteau, Sebastien, Furqan, Muhammad, Galaz, Gaspar, Gal-Yam, A., Garnavich, Peter, Gawiser, Eric, Geary, John, Gee, Perry, Gibson, Robert R., Gilmore, Kirk, Grace, Emily A., Green, Richard F., Gressler, William J., Grillmair, Carl J., Habib, Salman, Haggerty, J. S., Hamuy, Mario, Harris, Alan W., Hawley, Suzanne L., Heavens, Alan F., Hebb, Leslie, Henry, Todd J., Hileman, Edward, Hilton, Eric J., Hoadley, Keri, Holberg, J. B., Holman, Matt J., Howell, Steve B., Infante, Leopoldo, Ivezic, Zeljko, Jacoby, Suzanne H., Jain, Bhuvnesh, R, Jedicke, Jee, M. James, Garrett Jernigan, J., Jha, Saurabh W., Johnston, Kathryn V., Jones, R. Lynne, Juric, Mario, Kaasalainen, Mikko, Styliani, Kafka, Kahn, Steven M., Kaib, Nathan A., Kalirai, Jason, Kantor, Jeff, Kasliwal, Mansi M., Keeton, Charles R., Kessler, Richard, Knezevic, Zoran, Kowalski, Adam, Krabbendam, Victor L., Krughoff, K. Simon, Kulkarni, Shrinivas, Kuhlman, Stephen, Lacy, Mark, Lepine, Sebastien, Liang, Ming, Lien, Amy, Lira, Paulina, Long, Knox S., Lorenz, Suzanne, Lotz, Jennifer M., Lupton, R. H., Lutz, Julie, Macri, Lucas M., Mahabal, Ashish A., Mandelbaum, Rachel, Marshall, Phil, May, Morgan, Mcgehee, Peregrine M., Meadows, Brian T., Meert, Alan, Milani, Andrea, Miller, Christopher J., Miller, Michelle, Mills, David, Minniti, Dante, Monet, David, Mukadam, Anjum S., Nakar, Ehud, Neill, Douglas R., Newman, Jeffrey A., Nikolaev, Sergei, Nordby, Martin, O Connor, Paul, Oguri, Masamune, Oliver, John, Olivier, Scot S., Olsen, Julia K., Olsen, Knut, Olszewski, Edward W., Oluseyi, Hakeem, Padilla, Nelson D., Parker, Alex, Pepper, Joshua, Peterson, John R., Petry, Catherine, Pinto, Philip A., Pizagno, James L., Popescu, Bogdan, Prsa, Andrej, Radcka, Veljko, Raddick, M. Jordan, Rasmussen, Andrew, Rau, Arne, Rho, Jeonghee, Rhoads, James E., Richards, Gordon T., Ridgway, Stephen T., Robertson, Brant E., Roskar, Rok, Saha, Abhijit, Sarajedini, Ata, Scannapieco, Evan, Schalk, Terry, Schindler, Rafe, Schmidt, Samuel, Schmidt, Sarah, Schneider, Donald P., Schumacher, German, Scranton, Ryan, Sebag, Jacques, Seppala, Lynn G., Ohad Shemmer, Simon, Joshua D., Sivertz, M., Smith, Howard A., Allyn Smith, J., Smith, Nathan, Spitz, Anna H., Stanford, Adam, Stassun, Keivan G., Strader, Jay, Strauss, Michael A., Stubbs, Christopher W., Sweeney, Donald W., Szalay, Alex, Szkody, Paula, Takada, Masahiro, Thorman, Paul, Trilling, David E., Trimble, Virginia, Tyson, Anthony, Berg, Richard, Vanden Berk, Daniel, Vanderplas, Jake, Verde, Licia, Vrsnak, Bojan, Walkowicz, Lucianne M., Wandelt, Benjamin D., Wang, Sheng, Wang, Yun, Warner, Michael, Wechsler, Risa H., West, Andrew A., Wiecha, Oliver, Williams, Benjamin F., Willman, Beth, Wittman, David, Wolff, Sidney C., Wood-Vasey, W. Michael, Wozniak, Przemek, Young, Patrick, Zentner, Andrew, Zhan, Hu, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), LSST, Bartlett, James, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, Milky Way, FOS: Physical sciences, Large Synoptic Survey Telescope, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Weak gravitational lensing, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Astrophysics - Solar and Stellar Astrophysics, Sky, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics of Galaxies (astro-ph.GA), Dark energy, Instrumentation and Methods for Astrophysics, Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

A survey that can cover the sky in optical bands over wide fields to faint magnitudes with a fast cadence will enable many of the exciting science opportunities of the next decade. The Large Synoptic Survey Telescope (LSST) will have an effective aperture of 6.7 meters and an imaging camera with field of view of 9.6 deg^2, and will be devoted to a ten-year imaging survey over 20,000 deg^2 south of +15 deg. Each pointing will be imaged 2000 times with fifteen second exposures in six broad bands from 0.35 to 1.1 microns, to a total point-source depth of r~27.5. The LSST Science Book describes the basic parameters of the LSST hardware, software, and observing plans. The book discusses educational and outreach opportunities, then goes on to describe a broad range of science that LSST will revolutionize: mapping the inner and outer Solar System, stellar populations in the Milky Way and nearby galaxies, the structure of the Milky Way disk and halo and other objects in the Local Volume, transient and variable objects both at low and high redshift, and the properties of normal and active galaxies at low and high redshift. It then turns to far-field cosmological topics, exploring properties of supernovae to z~1, strong and weak lensing, the large-scale distribution of galaxies and baryon oscillations, and how these different probes may be combined to constrain cosmological models and the physics of dark energy., 596 pages. Also available at full resolution at http://www.lsst.org/lsst/scibook

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