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17 results on '"Melis, Carl"'

1. New chondritic bodies identified in eight oxygen-bearing white dwarfs

Author

Doyle, Alexandra E., Klein, Beth L., Dufour, Patrick, Melis, Carl, Zuckerman, B., Xu, Siyi, Weinberger, Alycia J., Trierweiler, Isabella L., Monson, Nathaniel N., Jura, Michael A., and Young, Edward D.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

We present observations and analyses of eight white dwarf stars that have accreted rocky material from their surrounding planetary systems. The spectra of these helium-atmosphere white dwarfs contain detectable optical lines of all four major rock-forming elements (O, Mg, Si, Fe). This work increases the sample of oxygen-bearing white dwarfs with parent body composition analyses by roughly thirty-three percent. To first order, the parent bodies that have been accreted by the eight white dwarfs are similar to those of chondritic meteorites in relative elemental abundances and oxidation states. Seventy-five percent of the white dwarfs in this study have observed oxygen excesses implying volatiles in the parent bodies with abundances similar to those of chondritic meteorites. Three white dwarfs have oxidation states that imply more reduced material than found in CI chondrites, indicating the possible detection of Mercury-like parent bodies, but are less constrained. These results contribute to the recurring conclusion that extrasolar rocky bodies closely resemble those in our solar system, and do not, as a whole, yield unusual or unique compositions., Comment: Accepted for publication in ApJ. 7 Figures, 7 Tables

Published
2023
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2. IRAS 00450+7401 and the mid-infrared fade/burst cycle of R Coronae Borealis-type stars

Author

Burris, William A., Melis, Carl, Shafter, Allen W., Panopoulou, Georgia V., Wright, Edward L., and Della Costa, John

Subjects
Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We present optical and infrared imaging and spectroscopy of the R Coronae Borealis-type (R Cor Bor) star IRAS 00450+7401. Optical spectra further confirm its classification as a cool R Cor Bor system, having a hydrogen-deficient carbon star spectral sub-class of HdC5 or later. Mid-infrared spectroscopy reveals the typical ~8 um ``hump'' seen in other R Cor Bor stars and no other features. A modern-epoch spectral energy distribution shows bright emission from hot dust having Tdust>600 K. Historical infrared data reveal generally cooler dust color temperatures combined with long-term fading trends, but provide no discernible correlation between flux level and temperature. Investigating the most mid-infrared variable R Cor Bor stars found in IRAS, AKARI, and WISE data reveals similar fading trends, bursts that can show a factor of up to 10 change in flux density between epochs, and blackbody-fit dust color temperatures that span 400-1300 K. While some R Cor Bor stars such as IRAS 00450+7401 appear to undergo fade/burst cycles in the mid-infrared, significant gaps in temporal coverage prevent conclusively identifying any preferred timescale for their mid-infrared variability and circumstellar dust temperature changes., AJ accepted, 15 pages, 6 figures, 5 tables, and an appendix

Published
2023
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3. An emerging and enigmatic spectral class of isolated DAe white dwarfs

Author

Elms, Abbigail K., Tremblay, Pier-Emmanuel, Gänsicke, Boris T., Swan, Andrew, Melis, Carl, Bédard, Antoine, Manser, Christopher J., Munday, James, Hermes, J. J., Dennihy, Erik, Nitta, Atsuko, and Zuckerman, Ben

Subjects
Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Two recently discovered white dwarfs, WDJ041246.84$+$754942.26 and WDJ165335.21$-$100116.33, exhibit H$\alpha$ and H$\beta$ Balmer line emission similar to stars in the emerging DAHe class, yet intriguingly have not been found to have detectable magnetic fields. These white dwarfs are assigned the spectral type DAe. We present detailed follow-up of the two known DAe stars using new time-domain spectroscopic observations and analysis of the latest photometric time-series data from TESS and ZTF. We measure the upper magnetic field strength limit of both stars as $B < 0.05$ MG. The DAe white dwarfs exhibit photometric and spectroscopic variability, where in the case of WDJ041246.84$+$754942.26 the strength of the H$\alpha$ and H$\beta$ emission cores varies in anti-phase with its photometric variability over the spin period, which is the same phase relationship seen in DAHe stars. The DAe white dwarfs closely cluster in one region of the Gaia Hertzsprung-Russell diagram together with the DAHe stars. We discuss current theories on non-magnetic and magnetic mechanisms which could explain the characteristics observed in DAe white dwarfs, but additional data are required to unambiguously determine the origin of these stars., Comment: 20 pages, 16 figures. Accepted for publication in MNRAS

Published
2023
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4. At what temperature does magnetic dynamo action cease? Or: How hot is the hottest cool star?

Author

Günther, Hans Moritz, Melis, Carl, Robrade, Jan, Schneider, Peter Christian, Wolk, Scott J., Yadav, Rakesh, Brun, Allan Sacha, Bouvier, Jérôme, and Petit, Pascal

Subjects
astronomy, stars, astrophysics, stellar activity, X-ray emission
Abstract

Cool stars on the main sequence generate X-rays from coronal activity, powered by a convective dynamo. With increasing temperature, the convective envelope becomes smaller and X-ray emission fainter, so some cool star must be the “hottest cool star” before emission ends. We present Chandra/HRC-I observations of four single stars with early A spectral types. Only the coolest star of this sample, \(\tau^3\) Eri (Teff = 8000 K), is detected with log(LX/Lbol)=-7.6, while the three hotter stars (Teff > 8100 K), namely \(\delta\) Leo, \(\beta\) Leo, and \(\iota\) Cen, remain undetected with upper limits log(LX/Lbol), {"references":["Simon, T., Ayres, T. R., Redfield, S., & Linsky, J. L. (2002), ApJ, 579, 800, doi: 10.1086/342941","Robrade, J., & Schmitt, J. H. M. M. (2010), A&A, 516, A38, doi: 10.1051/0004-6361/201014027","Robrade, J., & Schmitt, J. H. M. M. (2009), A&A, 497, 511, doi: 10.1051/0004-6361/200811348","Gu ̈nther, H. M., Wolk, S. J., Drake, J. J., et al. (2012), ApJ, 750, 78, doi: 10.1088/0004-637X/750/1/78","Pease, D. O., Drake, J. J., & Kashyap, V. L. (2006), ApJ, 636, 426, doi: 10.1086/497888","Drake, J. J., Braithwaite, J., Kashyap, V., Gu ̈nther, H. M., & Wright, N. J. (2014), ApJ, 786, 136, doi: 10.1088/0004-637X/786/2/136"]}

Published
2022
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5. Final Report for SAG 22: A Target Star Archive for Exoplanet Science

Author

Hinkel, Natalie R., Pepper, Joshua, Stark, Christopher C., Burt, Jennifer A., Ciardi, David R., Hardegree-Ullman, Kevin K., Lustig-Yaeger, Jacob, Kopparapu, Ravi, Mishra, Lokesh, Molaverdikhani, Karan, Pascucci, Ilaria, Richey-Yowell, Tyler, Safron, E. J., Wilson, David J., Bergsten, Galen, Boyajian, Tabetha S., Caballero, J. A., Cunha, K., Columbus, Alyssa, Domagal-Goldman, Shawn D., Dong, Chuanfei, Elowitz, R. M., Jha, Devanshu, Kalra, Archit, Latham, David W., Luhn, Jacob, Melis, Carl, Nagananda, Navya, Peretz, Eliad, Reffert, Sabine, Smith, Kimberly Scarangella, Stassun, Keivan G., Tanner, Angelle, Tuchow, Noah, Veras, Dimitri, and Winters, Jennifer G.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

Present and upcoming NASA missions will be intensively observing a selected, partially overlapping set of stars for exoplanet studies. Key physical and chemical information about these stars and their systems is needed for planning observations and interpreting the results. A target star archive of such data would benefit a wide cross-section of the exoplanet community by enhancing the chances of mission success and improving the efficiency of mission observatories. It would also provide a common, accessible resource for scientific analysis based on standardized assumptions, while revealing gaps or deficiencies in existing knowledge of stellar properties necessary for exoplanetary system characterization., Comment: main report: 25 pages including 5 tables and 3 figures; supplemental Appendices A-H also included (total 63 pages) with compiled materials and individual task force reports

Published
2021
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6. New Frontiers for Terrestrial-sized to Neptune-sized Exoplanets In the Era of Extremely Large Telescopes

Author

Wang, Ji, Meyer, Michael R., Boss, Alan, Close, Laird, Currie, Thayne, Dragomir, Diana, Fortney, Jonathan, Gaidos, Eric, Hasegawa, Yasuhiro, Kitiashvili, Irina, Konopacky, Quinn, Lee, Chien-Hsiu, Lewis, Nikole K., Liu, Michael, Lupu, Roxana, Mawet, Dimitri, Melis, Carl, Lopez-Morales, Mercedes, Morley, Caroline V., Packham, Chris, Peretz, Eliad, Skemer, Andy, and Ulmer, Mel

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Surveys reveal that terrestrial- to Neptune-sized planets (1 $< R, Comment: Astro2020 Science White Paper

Published
2019

7. White paper for Chandra cool attitude targets (CAT): Stellar activity with TESS and Chandra

Author

G��nther, Hans Moritz, Principe, David A., Melis, Carl, Monsch, Kristina, Schneider, P. Christian, Czesla, S., Wright, Nicholas J., Kashyap, Vinay L., Schmitt, J. H. M. M., Newton, E. R., Drake, Jeremy J., and Huenemoerder, D. P.

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

All cool stars show magnetic activity, and X-ray emission is the hallmark of this activity. Gaining an understanding of activity aids us in answering fundamental questions about stellar astrophysics and in determining the impact of activity on the exoplanets that orbit these stars. Stellar activity is driven by magnetic fields, which are ultimately powered by convection and stellar rotation. However, the resulting dynamo properties heavily depend on the stellar interior structure and are far from being understood. X-ray radiation can evaporate exoplanet atmospheres and damage organic materials on the planetary surface, reducing the probability that life can form or be sustained, but also provides an important source of energy for prebiotic chemical reactions. Over the next two years, the TESS mission will deliver a catalog of the closest exoplanets, along with rotation periods and activity diagnostics for millions of stars, whether or not they have a planet. We propose to include all cool stars that are TESS targets and bright enough for Chandra observations, as determined by their detection and flux in the ROSAT all-sky survey (RASS), to the list of Chandra Cool Attitude Targets (CATs). For each target, the signal will be sufficient to fit the coronal plasma with at least two temperature components, and compare abundances of groups of elements with low, medium, or high first ionization potential. Similar to the known relation between X-ray luminosity $L_X$ and rotation period, we can correlate stellar properties with coronal temperatures and abundances to constrain models for stellar activity, coronal heating, and stellar dynamos. Detailed X-ray characterization for even a subset of planet-hosting systems would dramatically advance our knowledge of what impact these emissions have on orbiting planets., White paper for Chandra cool attitude targets (4 pages)

Published
2019

8. Stellar Astrophysics and Exoplanet Science with the Maunakea Spectroscopic Explorer (MSE)

Author

Bergemann, Maria, Huber, Daniel, Adibekyan, Vardan, Angelou, George, Barría, Daniela, Beers, Timothy C., Beck, Paul G., Bellinger, Earl P., Bestenlehner, Joachim M., Bitsch, Bertram, Burgasser, Adam, Buzasi, Derek, Cassisi, Santi, Catelan, Márcio, Escorza, Ana, Fleming, Scott W., Gänsicke, Boris T., Gandolfi, Davide, García, Rafael A., Gieles, Mark, Karakas, Amanda, Lebreton, Yveline, Lodieu, Nicolas, Melis, Carl, Merle, Thibault, Mészáros, Szabolcs, Miglio, Andrea, Molaverdikhani, Karan, Monier, Richard, Morel, Thierry, Neilson, Hilding R., Oshagh, Mahmoudreza, Rybizki, Jan, Serenelli, Aldo, Smiljanic, Rodolfo, Szabó, Gyula M., Toonen, Silvia, Tremblay, Pier-Emmanuel, Valentini, Marica, Van Eck, Sophie, Zwintz, Konstanze, Bayo, Amelia, Cami, Jan, Casagrande, Luca, Gabdeev, Maksim, Gaulme, Patrick, Guiglion, Guillaume, Handler, Gerald, Hillenbrand, Lynne, Yildiz, Mutlu, Marley, Mark, Mosser, Benoit, Price-Whelan, Adrian M., Prsa, Andrej, Santisteban, Juan V. Hernández, Aguirre, Victor Silva, Sobeck, Jennifer, Stello, Dennis, Szabo, Robert, Tsantaki, Maria, Villaver, Eva, Wright, Nicholas J., Xu, Siyi, Zhang, Huawei, Anguiano, Borja, Bedell, Megan, Chaplin, Bill, Collet, Remo, Kamath, Devika, Martell, Sarah, Sousa, Sérgio G., Ting, Yuan-Sen, and Venn, Kim

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astronomie, Astrophysique, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

The Maunakea Spectroscopic Explorer (MSE) is a planned 11.25-m aperture facility with a 1.5 square degree field of view that will be fully dedicated to multi-object spectroscopy. A rebirth of the 3.6m Canada-France-Hawaii Telescope on Maunakea, MSE will use 4332 fibers operating at three different resolving powers (R ~ 2500, 6000, 40000) across a wavelength range of 0.36-1.8mum, with dynamical fiber positioning that allows fibers to match the exposure times of individual objects. MSE will enable spectroscopic surveys with unprecedented scale and sensitivity by collecting millions of spectra per year down to limiting magnitudes of g ~ 20-24 mag, with a nominal velocity precision of ~100 m/s in high-resolution mode. This white paper describes science cases for stellar astrophysics and exoplanet science using MSE, including the discovery and atmospheric characterization of exoplanets and substellar objects, stellar physics with star clusters, asteroseismology of solar-like oscillators and opacity-driven pulsators, studies of stellar rotation, activity, and multiplicity, as well as the chemical characterization of AGB and extremely metal-poor stars., Comment: 31 pages, 11 figures; To appear as a chapter for the Detailed Science Case of the Maunakea Spectroscopic Explorer

Published
2019
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9. Astro 2020 Science White Paper: Evolved Planetary Systems around White Dwarfs

Author

Gaensicke, Boris, Barstow, Martin, Bonsor, Amy, Debes, John, Dufour, Patrick, Cunningham, Tim, Dennihy, Erik, Fusillo, Nicola Gentile, Farihi, Jay, Hollands, Mark, Hoskin, Matthew, Izquierdo, Paula, Johnson, Jennifer, Klein, Beth, Koester, Detlev, Kollmeier, Juna, Lyra, Wladimir, Manser, Christopher, Melis, Carl, Rodriguez-Gil, Pablo, Schreiber, Matthias, Swan, Andrew, Toloza, Odette, Tremblay, Pier-Emmanuel, Veras, Dimitri, Wilson, David, Xu, Siyi, and Zuckerman, Ben

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Practically all known planet hosts will evolve into white dwarfs, and large parts of their planetary systems will survive this transition - the same is true for the solar system beyond the orbit of Mars. Spectroscopy of white dwarfs accreting planetary debris provides the most accurate insight into the bulk composition of exo-planets. Ground-based spectroscopic surveys of ~260, 000 white dwarfs detected with Gaia will identify >1000 evolved planetary systems, and high-throughput high-resolution space-based ultraviolet spectroscopy is essential to measure in detail their abundances. So far, evidence for two planetesimals orbiting closely around white dwarfs has been obtained, and their study provides important constraints on the composition and internal structure of these bodies. Major photometric and spectroscopic efforts will be necessary to assemble a sample of such close-in planetesimals that is sufficiently large to establish their properties as a population, and to deduce the architectures of the outer planetary systems from where they originated. Mid-infrared spectroscopy of the dusty disks will provide detailed mineralogical information of the debris, which, in combination with the elemental abundances measured from the white dwarf spectroscopy, will enable detailed physical modelling of the chemical, thermodynamic, and physical history of the accreted material. Flexible multi-epoch infrared observations are essential to determine the physical nature, and origin of the variability observed in many of the dusty disks. Finally, the direct detection of the outer reservoirs feeding material to the white dwarfs will require sensitive mid- and far-infrared capabilities., 5 pages, 3 figures Science White Paper submitted to the Astro2020 Decadal Survey

Published
2019
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10. The Detailed Science Case for the Maunakea Spectroscopic Explorer, 2019 edition

Author

The MSE Science Team, Babusiaux, Carine, Bergemann, Maria, Burgasser, Adam, Ellison, Sara, Haggard, Daryl, Huber, Daniel, Kaplinghat, Manoj, Li, Ting, Marshall, Jennifer, Martell, Sarah, McConnachie, Alan, Percival, Will, Robotham, Aaron, Shen, Yue, Thirupathi, Sivarani, Tran, Kim-Vy, Yeche, Christophe, Yong, David, Adibekyan, Vardan, Aguirre, Victor Silva, Angelou, George, Asplund, Martin, Balogh, Michael, Banerjee, Projjwal, Bannister, Michele, Barría, Daniela, Battaglia, Giuseppina, Bayo, Amelia, Bechtol, Keith, Beck, Paul G., Beers, Timothy C., Bellinger, Earl P., Berg, Trystyn, Bestenlehner, Joachim M., Bilicki, Maciej, Bitsch, Bertram, Bland-Hawthorn, Joss, Bolton, Adam S., Boselli, Alessandro, Bovy, Jo, Bragaglia, Angela, Buzasi, Derek, Caffau, Elisabetta, Cami, Jan, Carleton, Timothy, Casagrande, Luca, Cassisi, Santi, Catelan, Márcio, Chang, Chihway, Cortese, Luca, Damjanov, Ivana, Davies, Luke J. M., de Grijs, Richard, de Rosa, Gisella, Deason, Alis, di Matteo, Paola, Drlica-Wagner, Alex, Erkal, Denis, Escorza, Ana, Ferrarese, Laura, Fleming, Scott W., Font-Ribera, Andreu, Freeman, Ken, Gänsicke, Boris T., Gabdeev, Maksim, Gallagher, Sarah, Gandolfi, Davide, García, Rafael A., Gaulme, Patrick, Geha, Marla, Gennaro, Mario, Gieles, Mark, Gilbert, Karoline, Gordon, Yjan, Goswami, Aruna, Greco, Johnny P., Grillmair, Carl, Guiglion, Guillaume, Hénault-Brunet, Vincent, Hall, Patrick, Handler, Gerald, Hansen, Terese, Hathi, Nimish, Hatzidimitriou, Despina, Haywood, Misha, Santisteban, Juan V. Hernández, Hillenbrand, Lynne, Hopkins, Andrew M., Howlett, Cullan, Hudson, Michael J., Ibata, Rodrigo, Ilić, Dragana, Jablonka, Pascale, Ji, Alexander, Jiang, Linhua, Juneau, Stephanie, Karakas, Amanda, Karinkuzhi, Drisya, Kim, Stacy Y., Kong, Xu, Konstantopoulos, Iraklis, Krogager, Jens-Kristian, Lagos, Claudia, Lallement, Rosine, Laporte, Chervin, Lebreton, Yveline, Lee, Khee-Gan, Lewis, Geraint F., Lianou, Sophia, Liu, Xin, Lodieu, Nicolas, Loveday, Jon, Mészáros, Szabolcs, Makler, Martin, Mao, Yao-Yuan, Marchesini, Danilo, Martin, Nicolas, Mateo, Mario, Melis, Carl, Merle, Thibault, Miglio, Andrea, Mohammad, Faizan Gohar, Molaverdikhani, Karan, Monier, Richard, Morel, Thierry, Mosser, Benoit, Nataf, David, Necib, Lina, Neilson, Hilding R., Newman, Jeffrey A., Nierenberg, A. M., Nord, Brian, Noterdaeme, Pasquier, O'Dea, Chris, Oshagh, Mahmoudreza, Pace, Andrew B., Palanque-Delabrouille, Nathalie, Pandey, Gajendra, Parker, Laura C., Pawlowski, Marcel S., Peter, Annika H. G., Petitjean, Patrick, Petric, Andreea, Placco, Vinicius, Popović, Luka Č., Price-Whelan, Adrian M., Prsa, Andrej, Ravindranath, Swara, Rich, R. Michael, Ruan, John, Rybizki, Jan, Sakari, Charli, Sanderson, Robyn E., Schiavon, Ricardo, Schimd, Carlo, Serenelli, Aldo, Siebert, Arnaud, Siudek, Malgorzata, Smiljanic, Rodolfo, Smith, Daniel, Sobeck, Jennifer, Starkenburg, Else, Stello, Dennis, Szabó, Gyula M., Szabo, Robert, Taylor, Matthew A., Thanjavur, Karun, Thomas, Guillaume, Tollerud, Erik, Toonen, Silvia, Tremblay, Pier-Emmanuel, Tresse, Laurence, Tsantaki, Maria, Valentini, Marica, Van Eck, Sophie, Variu, Andrei, Venn, Kim, Villaver, Eva, Walker, Matthew G., Wang, Yiping, Wang, Yuting, Wilson, Michael J., Wright, Nicolas, Xu, Siyi, Yildiz, Mutlu, Zhang, Huawei, Zwintz, Konstanze, Anguiano, Borja, Bedell, Megan, Chaplin, William, Collet, Remo, Cuillandre, Jean-Charles, Duc, Pierre-Alain, Flagey, Nicolas, Hermes, JJ, Hill, Alexis, Kamath, Devika, Laychak, Mary Beth, Małek, Katarzyna, Marley, Mark, Sheinis, Andy, Simons, Doug, Sousa, Sérgio G., Szeto, Kei, Ting, Yuan-Sen, Vegetti, Simona, Wells, Lisa, Babas, Ferdinand, Bauman, Steve, Bosselli, Alessandro, Côté, Pat, Colless, Matthew, Comparat, Johan, Courtois, Helene, Crampton, David, Croom, Scott, Davies, Luke, Denny, Kelly, Devost, Daniel, Driver, Simon, Fernandez-Lorenzo, Mirian, Guhathakurta, Raja, Han, Zhanwen, Higgs, Clare, Hill, Vanessa, Ho, Kevin, Hopkins, Andrew, Hudson, Mike, Isani, Sidik, Jarvis, Matt, Johnson, Andrew, Jullo, Eric, Kaiser, Nick, Kneib, Jean-Paul, Koda, Jun, Koshy, George, Mignot, Shan, Murowinski, Rick, Newman, Jeff, Nusser, Adi, Pancoast, Anna, Peng, Eric, Peroux, Celine, Pichon, Christophe, Poggianti, Bianca, Richard, Johan, Salmon, Derrick, Seibert, Arnaud, Shastri, Prajval, Smith, Dan, Sutaria, Firoza, Tao, Charling, Taylor, Edwar, Tully, Brent, van Waerbeke, Ludovic, Vermeulen, Tom, Walker, Matthew, Willis, Jon, Willot, Chris, Withington, Kanoa, International Max Planck Research School for Astronomy and Cosmic Physics (University of Heidelberg), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Center for Astrophysics and Space Sciences [La Jolla] (CASS), University of California [San Diego] (UC San Diego), University of California-University of California, Cognition, Langues, Langage, Ergonomie (CLLE-ERSS), École pratique des hautes études (EPHE)-Université Toulouse - Jean Jaurès (UT2J)-Université Bordeaux Montaigne-Centre National de la Recherche Scientifique (CNRS), Technicolor R & I [Cesson Sévigné], Technicolor, University of Edinburgh, University of Texas-Pan American (UTPA), University of Texas-Pan, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Australian National University (ANU), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Max-Planck-Institut für Astronomie (MPIA), Lund Observatory, Lund University [Lund], Anglo-Australian Observatory (AAO), 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), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], Department of Physics and Astronomy [London, ON], University of Western Ontario (UWO), National Research Council of Canada (NRC), STScI, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy, University of Cambridge [UK] (CAM), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), State Key Laboratory of Fine Chemicals, Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), School of Physics and Astronomy, University of Birmingham [Birmingham], Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Sciences, Philosophie, Histoire (SPHERE UMR 7219), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [UCLA Los Angeles], University of California [Los Angeles] (UCLA), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], High Speed Networks Laboratory, Dept. of Telecommunications and Media Informatics, Budapest University of Technology and Economics [Budapest] (BME), Laboratoire Interdisciplinaire Carnot de Bourgogne (LICB), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, College of Life Sciences, Peking Univertsity, Department of Mathematics [UCLA], Department of Psychology, St John's University, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), 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), Herzberg Institute of Astrophysics, Department of electronic engineering, Chang Gung University, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), The Open Group Research Institute (TOGRI), Université Joseph Fourier - Grenoble 1 (UJF), École normale supérieure - Paris (ENS Paris), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), MSE Science Team, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J)-Université Bordeaux Montaigne-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Cambridge], Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Sciences, Philosophie, Histoire (SPHERE (UMR_7219)), 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), Université Paris sciences et lettres (PSL), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Aix Marseille Université (AMU)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Bourgogne (UB), University of California (UC)-University of California (UC), École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Bordeaux Montaigne (UBM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Universität Heidelberg [Heidelberg] = Heidelberg University, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interdisciplinaire Carnot de Bourgogne (ICB), Peking University [Beijing], Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Universidad Autónoma de Madrid (UAM), École normale supérieure - Paris (ENS-PSL), 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), and Lebreton, Yveline

Subjects
[PHYS]Physics [physics], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, [PHYS] Physics [physics], [SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(Abridged) The Maunakea Spectroscopic Explorer (MSE) is an end-to-end science platform for the design, execution and scientific exploitation of spectroscopic surveys. It will unveil the composition and dynamics of the faint Universe and impact nearly every field of astrophysics across all spatial scales, from individual stars to the largest scale structures in the Universe. Major pillars in the science program for MSE include (i) the ultimate Gaia follow-up facility for understanding the chemistry and dynamics of the distant Milky Way, including the outer disk and faint stellar halo at high spectral resolution (ii) galaxy formation and evolution at cosmic noon, via the type of revolutionary surveys that have occurred in the nearby Universe, but now conducted at the peak of the star formation history of the Universe (iii) derivation of the mass of the neutrino and insights into inflationary physics through a cosmological redshift survey that probes a large volume of the Universe with a high galaxy density. MSE is positioned to become a critical hub in the emerging international network of front-line astronomical facilities, with scientific capabilities that naturally complement and extend the scientific power of Gaia, the Large Synoptic Survey Telescope, the Square Kilometer Array, Euclid, WFIRST, the 30m telescopes and many more., 9 chapters, 301 pages, 100 figures. This version of the DSC is a comprehensive update of the original version, released in 2016, which can be downloaded at arXiv:1606.00043. A detailed summary of the design of MSE is available in the MSE Book 2018, available at arXiv:1810.08695

Published
2019

11. The first polluted white dwarf from Gaia DR2: the cool DAZ GaiaJ1738-0826

Author

Melis, Carl, Zuckerman, B., Dufour, P., Song, I., and Klein, B.

Subjects
Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We present the first metal-polluted single white dwarf star identified through Gaia DR2. GaiaJ1738-0826, selected from color and absolute magnitude cuts in the Gaia DR2 data, was discovered to have strong Ca~II absorption in initial spectroscopic characterization at Lick Observatory. Notably, GaiaJ1738-0826 resembles in many ways the first confirmed metal-polluted hydrogen atmosphere white dwarf, the DAZ G74-7., 3 pages, 1 figure. Accepted for publication in RNAAS

Published
2018

12. Thirty Meter Telescope Detailed Science Case: 2015

Author

Skidmore, Warren, Dell'Antonio, Ian, Fukugawa, Misato, Goswami, Aruna, Hao, Lei, Jewitt, David, Laughlin, Greg, Steidel, Charles, Hickson, Paul, Simard, Luc, Sch��ck, Matthias, Treu, Tommaso, Cohen, Judith, Anupama, G. C., Dickinson, Mark, Harrison, Fiona, Kodama, Tadayuki, Lu, Jessica R., Macintosh, Bruce, Malkan, Matt, Mao, Shude, Narita, Norio, Sekiguchi, Tomohiko, Subramaniam, Annapurni, Tanaka, Masaomi, Tian, Feng, A'Hearn, Michael, Akiyama, Masayuki, Ali, Babar, Aoki, Wako, Bagchi, Manjari, Barth, Aaron, Bhalerao, Varun, Bradac, Marusa, Bullock, James, Burgasser, Adam J., Chapman, Scott, Chary, Ranga-Ram, Chiba, Masashi, Cooper, Michael, Cooray, Asantha, Crossfield, Ian, Currie, Thayne, Das, Mousumi, Dewangan, G. C., de Grijs, Richard, Do, Tuan, Dong, Subo, Evslin, Jarah, Fang, Taotao, Fang, Xuan, Fassnacht, Christopher, Fletcher, Leigh, Gaidos, Eric, Gal, Roy, Ghez, Andrea, Giavalisco, Mauro, Grady, Carol A., Greathouse, Thomas, Gogoi, Rupjyoti, Guhathakurta, Puragra, Ho, Luis, Hasan, Priya, Herczeg, Gregory J., Honda, Mitsuhiko, Imanishi, Masa, Inami, Hanae, Iye, Masanori, Kalirai, Jason, Kamath, U. S., Kane, Stephen, Kashikawa, Nobunari, Kasliwal, Mansi, Kasliwal, Vishal, Kirby, Evan, Konopacky, Quinn M., Lepine, Sebastien, Li, Di, Li, Jianyang, Liu, Junjun, Liu, Michael C., Lopez-Rodriguez, Enrigue, Lotz, Jennifer, Lubin, Philip, Macri, Lucas, Maeda, Keiichi, Marchis, Franck, Marois, Christian, Marscher, Alan, Martin, Crystal, Matsuo, Taro, Max, Claire, McConnachie, Alan, McGough, Stacy, Melis, Carl, Meyer, Leo, Mumma, Michael, Muto, Takayuki, Nagao, Tohru, Najita, Joan R., Navarro, Julio, Pierce, Michael, Prochaska, Jason X., Oguri, Masamune, Ojha, Devendra K., Okamoto, Yoshiko K., Orton, Glenn, Otarola, Angel, Ouchi, Masami, Packham, Chris, Padgett, Deborah L., Pandey, Shashi Bhushan, Pilachowsky, Catherine, Pontoppidan, Klaus M., Primack, Joel, Puthiyaveettil, Shalima, Ramirez-Ruiz, Enrico, Reddy, Naveen, Rich, Michael, Richter, Matthew J., Schombert, James, Sen, Anjan Ananda, Shi, Jianrong, Sheth, Kartik, Srianand, R., Tan, Jonathan C., Tanaka, Masayuki, Tanner, Angelle, Tominaga, Nozomu, Tytler, David, U, Vivian, Wang, Lingzhi, Wang, Xiaofeng, Wang, Yiping, Wilson, Gillian, Wright, Shelley, Wu, Chao, Wu, Xufeng, Xu, Renxin, Yamada, Toru, Yang, Bin, Zhao, Gongbo, and Zhao, Hongsheng

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Library science, Astrophysics, 01 natural sciences, 7. Clean energy, Cosmology, Observatory, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Cosmological model, Astrophysics - Astrophysics of Galaxies, Chinese academy of sciences, Exoplanet, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), General partnership, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Thirty Meter Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The TMT Detailed Science Case describes the transformational science that the Thirty Meter Telescope will enable. Planned to begin science operations in 2024, TMT will open up opportunities for revolutionary discoveries in essentially every field of astronomy, astrophysics and cosmology, seeing much fainter objects much more clearly than existing telescopes. Per this capability, TMT's science agenda fills all of space and time, from nearby comets and asteroids, to exoplanets, to the most distant galaxies, and all the way back to the very first sources of light in the Universe. More than 150 astronomers from within the TMT partnership and beyond offered input in compiling the new 2015 Detailed Science Case. The contributing astronomers represent the entire TMT partnership, including the California Institute of Technology (Caltech), the Indian Institute of Astrophysics (IIA), the National Astronomical Observatories of the Chinese Academy of Sciences (NAOC), the National Astronomical Observatory of Japan (NAOJ), the University of California, the Association of Canadian Universities for Research in Astronomy (ACURA) and US associate partner, the Association of Universities for Research in Astronomy (AURA)., Comment: 203 pages, 10 Mb. Full resolution version available at http://www.tmt.org/science-case/

Published
2015
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13. The bulk composition of exo-planets

Author

Boris Gaensicke, Debes, John, Dufour, Patrick, Farihi, Jay, Jura, Michael, Kilic, Mukremin, Melis, Carl, Veras, Dimitri, Xu, Siyi, and Zuckerman, Ben

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

Priorities in exo-planet research are rapidly moving from finding planets to characterizing their physical properties. Of key importance is their chemical composition, which feeds back into our understanding of planet formation. For the foreseeable future, far-ultraviolet spectroscopy of white dwarfs accreting planetary debris remains the only way to directly and accurately measure the bulk abundances of exo-planetary bodies. The exploitation of this method is limited by the sensitivity of HST, and significant progress will require a large-aperture space telescope with a high-throughput ultraviolet spectrograph., Comment: Submitted in response to NASA call for white papers: "Large Astrophysics Missions to Be Studied by NASA Prior to the 2020 Decadal Survey"

Published
2015
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14. Bridging the gap on tight separation brown dwarf binaries

Author

Gagliuffi, Daniella C. Bardalez, Burgasser, Adam J., Gelino, Christopher R., Melis, Carl, and Blake, Cullen

Subjects
Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Multiplicity is a key statistic for understanding the formation of very low mass (VLM) stars and brown dwarfs. Currently, the separation distribution of VLM binaries remains poorly constrained at small separations (

Published
2014

15. Cool Star Science with the FIRE Spectrograph

Author

Burgasser, Adam J., Simcoe, Robert A., Bochanski, John J., Melis, Carl, McMurtry, Craig, Pipher, Judy, Forrest, William, Cushing, Michael C., Looper, Dagny L., and Mohanty, Subhanjoy

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Folded-port InfraRed Echellette (FIRE) has recently been commissioned on the Magellan 6.5m Baade Telescope. This single object, near-infrared spectrometer simultaneously covers the 0.85-2.45 micron window in both cross-dispersed (R ~ 6000) or prism-dispersed (R ~ 250-350) modes. FIRE's compact configuration, high transmission optics and high quantum efficiency detector provides considerable sensitivity in the near-infrared, making it an ideal instrument for studies of cool stars and brown dwarfs. Here we present some of the first cool star science results with FIRE based on commissioning and science verification observations, including evidence of clouds in a planetary-mass brown dwarf, accretion and jet emission in the low-mass T Tauri star TWA 30B, radial velocities of T-type brown dwarfs, and near-infrared detection of a debris disk associated with the DAZ white dwarf GALEX 1931+01., 8 pages in ASP format, contribution to Proceedings of the 16th Cool Stars, Stellar Systems and the Sun (eds. C. Johns-Krull, M. Browning & A. West)

Published
2010

16. Metal Absorption Systems in Spectra of Pairs of QSOs

Author

Tytler, David, Gleed, Mark, Melis, Carl, Chapman, Angela, Kirkman, David, Lubin, Dan, Paschos, Pascal, Jena, Tridivesh, and Crotts, Arlin P. S.

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

We present the first large sample of absorption systems in paired QSOs consisting of 691 absorption systems in the spectra of 310 QSOs including 170 pairings. All these absorption systems have metal lines, usually C IV or Mg II. We see 17 cases of absorption in one line-of-sight within 200 km/s (1 Mpc) of absorption in the paired line-of-sight with the probability at least approx 50% at 100kpc, declining rapidly to 23% at 100 - 200 kpc. We detect clustering on 0.5Mpc scales and see a hint of the "fingers of God" redshift-space distortion. The distribution matches absorbers arising in galaxies at z=2 with a normal correlation function and systematic infall velocities but unusually low random pair-wise velocity differences. Absorption in gas flowing out from galaxies at a mean velocity of 250 km/s would produce vastly more elongation than we see. The UV absorption from fast winds that Adelberger et al. 2005 see in spectra of LBGs is not representative of the absorption that we see. Either the winds are confined to LBGs, or they can not extend to 40 kpc with large velocities, while continuing to make UV absorption we see, implying most metals were in place in the IGM long before z=2. Separately, when we examine the absorption seen when a sight line passes a second QSO, we see 19 absorbers within 400 km/s of the partner QSO. The probability of seeing absorption is approximately constant for impact parameters 0.1 - 1.5 Mpc. Perhaps we do not see a rapid rise in the probability at small impact parameters because the UV from QSOs destroys some absorbers near to the QSOs. The 3D distribution of 64 absorbers around 313 QSOs is to first order isotropic, with just a hint of the anisotropy expected if the QSO UV emission is beamed, or alternatively QSOs might emit UV isotropically but for a surprisingly short time of only 0.3Myr., Comment: 36 pages with 25 figures and 10 Tables Submited to MNRAS

Published
2007
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17. The H I opacity of the intergalactic medium at redshifts 1.6 < z < 3.2

Author

Kirkman, David, Tytler, David, Suzuki, Nao, Melis, Carl, Hollywood, Susan, James, Kory, So, Geoffrey, Lubin, Dan, Jena, Tridivesh, Norman, Michael L., and Paschos, Pascal

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

We use high quality echelle spectra of 24 QSOs to provide a calibrated measurement of the total amount of Lyman-alpha forest absorption (DA) over the redshift range 2.2 < z < 3.2. Our measurement of DA excludes absorption from metal lines or the Lyman-alpha lines of Lyman limit systems and damped Lyman-alpha systems. We use artificial spectra with realistic flux calibration errors to show that we are able to place continuum levels that are accurate to better than 1%. When we combine our results with our previous results between 1.6 < z < 2.2, we find that the redshift evolution of DA is well described over 1.6 < z < 3.2 as A*(1+z)^gamma, where A = 0.0062 and gamma = 2.75. We detect no significant deviations from a smooth power law evolution over the redshift range studied. We find less H I absorption than expected at z=3, implying that the UV background is about 40% higher than expected. Our data appears to be consistent with an H I ionization rate of Gamma ~ 1.4E-12 1/s., Accepted for publication in MNRAS

Published
2005
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