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104. SMASH 1: A VERY FAINT GLOBULAR CLUSTER DISRUPTING IN THE OUTER REACHES OF THE LMC?

Author

Martin, Nicolas F., primary, Jungbluth, Valentin, additional, Nidever, David L., additional, Bell, Eric F., additional, Besla, Gurtina, additional, Blum, Robert D., additional, Cioni, Maria-Rosa L., additional, Conn, Blair C., additional, Kaleida, Catherine C., additional, Gallart, Carme, additional, Jin, Shoko, additional, Majewski, Steven R., additional, Martinez-Delgado, David, additional, Monachesi, Antonela, additional, Muñoz, Ricardo R., additional, Noël, Noelia E. D., additional, Olsen, Knut, additional, Stringfellow, Guy S., additional, van der Marel, Roeland P., additional, Vivas, A. Katherina, additional, Walker, Alistair R., additional, and Zaritsky, Dennis, additional

Published
2016
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107. Extragalactic archeology with the GHOSTS Survey

Author

Streich, David, primary, de Jong, Roelof S., additional, Bailin, Jeremy, additional, Bell, Eric F., additional, Holwerda, Benne W., additional, Minchev, Ivan, additional, Monachesi, Antonela, additional, and Radburn-Smith, David J., additional

Published
2015
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108. PANCHROMATIC HUBBLE ANDROMEDA TREASURY. XII. MAPPING STELLAR METALLICITY DISTRIBUTIONS IN M31

Author

Gregersen, Dylan, primary, Seth, Anil C., additional, Williams, Benjamin F., additional, Lang, Dustin, additional, Dalcanton, Julianne J., additional, Girardi, Leó, additional, Skillman, Evan D., additional, Bell, Eric, additional, Dolphin, Andrew E., additional, Fouesneau, Morgan, additional, Guhathakurta, Puragra, additional, Hamren, Katherine M., additional, Johnson, L. C., additional, Kalirai, Jason, additional, R. Lewis, Alexia, additional, Monachesi, Antonela, additional, and Olsen, Knut, additional

Published
2015
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110. A GLOBAL STAR-FORMING EPISODE IN M31 2–4 GYR AGO

Author

Williams, Benjamin F., primary, Dalcanton, Julianne J., additional, Dolphin, Andrew E., additional, Weisz, Daniel R., additional, Lewis, Alexia R., additional, Lang, Dustin, additional, Bell, Eric F., additional, Boyer, Martha, additional, Fouesneau, Morgan, additional, Gilbert, Karoline M., additional, Monachesi, Antonela, additional, and Skillman, Evan, additional

Published
2015
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111. THE PANCHROMATICHUBBLEANDROMEDA TREASURY. XI. THE SPATIALLY RESOLVED RECENT STAR FORMATION HISTORY OF M31

Author

Lewis, Alexia R., primary, Dolphin, Andrew E., additional, Dalcanton, Julianne J., additional, Weisz, Daniel R., additional, Williams, Benjamin F., additional, Bell, Eric F., additional, Seth, Anil C., additional, Simones, Jacob E., additional, Skillman, Evan D., additional, Choi, Yumi, additional, Fouesneau, Morgan, additional, Guhathakurta, Puragra, additional, Johnson, Lent C., additional, Kalirai, Jason S., additional, Leroy, Adam K., additional, Monachesi, Antonela, additional, Rix, Hans-Walter, additional, and Schruba, Andreas, additional

Published
2015
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112. HYDRA II: A FAINT AND COMPACT MILKY WAY DWARF GALAXY FOUND IN THE SURVEY OF THE MAGELLANIC STELLAR HISTORY

Author

Martin, Nicolas F., primary, Nidever, David L., additional, Besla, Gurtina, additional, Olsen, Knut, additional, Walker, Alistair R., additional, Vivas, A. Katherina, additional, Gruendl, Robert A., additional, Kaleida, Catherine C., additional, Muñoz, Ricardo R., additional, Blum, Robert D., additional, Saha, Abhijit, additional, Conn, Blair C., additional, Bell, Eric F., additional, Chu, You-Hua, additional, Cioni, Maria-Rosa L., additional, Boer, Thomas J. L. de, additional, Gallart, Carme, additional, Jin, Shoko, additional, Kunder, Andrea, additional, Majewski, Steven R., additional, Martinez-Delgado, David, additional, Monachesi, Antonela, additional, Monelli, Matteo, additional, Monteagudo, Lara, additional, Noël, Noelia E. D., additional, Olszewski, Edward W., additional, Stringfellow, Guy S., additional, Marel, Roeland P. van der, additional, and Zaritsky, Dennis, additional

Published
2015
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113. THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. X. ULTRAVIOLET TO INFRARED PHOTOMETRY OF 117 MILLION EQUIDISTANT STARS

Author

Williams, Benjamin F., primary, Lang, Dustin, additional, Dalcanton, Julianne J., additional, Dolphin, Andrew E., additional, Weisz, Daniel R., additional, Bell, Eric F., additional, Bianchi, Luciana, additional, Byler, Nell, additional, Gilbert, Karoline M., additional, Girardi, Léo, additional, Gordon, Karl, additional, Gregersen, Dylan, additional, Johnson, L. C., additional, Kalirai, Jason, additional, Lauer, Tod R., additional, Monachesi, Antonela, additional, Rosenfield, Philip, additional, Seth, Anil, additional, and Skillman, Eva, additional

Published
2014
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114. Supplementary online material for article, "THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. X. ULTRAVIOLET TO INFRARED PHOTOMETRY OF 117 MILLION EQUIDISTANT STARS"

Author

Williams, Benjamin F, primary, Lang, Dustin, additional, Dalcanton, Julian J, additional, Dolphin, Andrew E, additional, Weisz, Daniel R, additional, Bell, Eric F, additional, Bianchi, Luciana, additional, Byler, Nell, additional, Gilbert, Karoline M, additional, Giradi, L'eo, additional, Gordon, Karl, additional, Gregersen, Dylan, additional, Johnson, LC, additional, Kalirai, Jason, additional, Lauer, Tod R, additional, Monachesi, Antonela, additional, Rosenfield, Philip, additional, Seth, Anil, additional, and Skillman, Eva, additional

Published
2014
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115. WiNDS: An H α Kinematics Survey of Nearby Spiral Galaxiesâ€"Vertical Perturbations in Nearby Disk-type Galaxies.

Author

Urrejola-Mora, Catalina, Gómez, Facundo A., Torres-Flores, Sergio, Amram, Philippe, Epinat, Benoît, Monachesi, Antonela, Marinacci, Federico, and de Oliveira, Claudia Mendes

Subjects
DISK galaxies, KINEMATICS, GALAXIES, MILKY Way, DATA libraries
Abstract

We present the Waves in Nearby Disk galaxies Survey (WiNDS) consisting of 40 nearby low-inclination disk galaxies observed through H α high-resolution Fabryâ€"Perot interferometry. WiNDS consists of 12 new galaxy observations and 28 data archived observations obtained from different galaxy surveys. We derive two-dimensional line-of-sight velocity fields that are analyzed to identify the possible presence of vertical velocity flows in the galactic disks of these low-inclination late-type galaxies using velocity residual maps, derived from the subtraction of an axisymmetric rotation model from a rotational velocity map. Large and globally coherent flows in the line-of-sight velocity of nearly face-on galaxies can be associated with large vertical displacement of the disk with respect to its midplane. Our goal is to characterize how frequent vertical perturbations, such as those observed in the Milky Way, arise in the local universe. Our currently available data have allowed us to identify 20% of WiNDS galaxies with strong velocity perturbations that are consistent with vertically perturbed galactic disks. [ABSTRACT FROM AUTHOR]

Published
2022
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116. GHOSTS I: A NEW FAINT VERY ISOLATED DWARF GALAXY ATD= 12 ± 2 Mpc

Author

Monachesi, Antonela, primary, Bell, Eric F., additional, Radburn-Smith, David J., additional, de Jong, Roelof S., additional, Bailin, Jeremy, additional, Dalcanton, Julianne J., additional, Holwerda, Benne W., additional, Alyson Ford, H., additional, Streich, David, additional, Vlajić, Marija, additional, and Zucker, Daniel B., additional

Published
2013
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120. PHAT STELLAR CLUSTER SURVEY. I. YEAR 1 CATALOG AND INTEGRATED PHOTOMETRY

Author

Johnson, L. Clifton, primary, Seth, Anil C., additional, Dalcanton, Julianne J., additional, Caldwell, Nelson, additional, Fouesneau, Morgan, additional, Gouliermis, Dimitrios A., additional, Hodge, Paul W., additional, Larsen, Søren S., additional, Olsen, Knut A. G., additional, San Roman, Izaskun, additional, Sarajedini, Ata, additional, Weisz, Daniel R., additional, Williams, Benjamin F., additional, Beerman, Lori C., additional, Bianchi, Luciana, additional, Dolphin, Andrew E., additional, Girardi, Léo, additional, Guhathakurta, Puragra, additional, Kalirai, Jason, additional, Lang, Dustin, additional, Monachesi, Antonela, additional, Nanda, Sanjay, additional, Rix, Hans-Walter, additional, and Skillman, Evan D., additional

Published
2012
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121. THE STAR FORMATION HISTORY OF M32

Author

Monachesi, Antonela, primary, Trager, Scott C., additional, Lauer, Tod R., additional, Hidalgo, Sebastián L., additional, Freedman, Wendy, additional, Dressler, Alan, additional, Grillmair, Carl, additional, and Mighell, Kenneth J., additional

Published
2012
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123. RR LYRAE VARIABLES IN M32 AND THE DISK OF M31

Author

Fiorentino, Giuliana, primary, Monachesi, Antonela, additional, Trager, Scott C., additional, Lauer, Tod R., additional, Saha, Abhijit, additional, Mighell, Kenneth J., additional, Freedman, Wendy, additional, Dressler, Alan, additional, Grillmair, Carl, additional, and Tolstoy, Eline, additional

Published
2009
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125. M32: Is there an Ancient and Metal-poor Stellar Population?

Author

Fiorentino, Giuliana, primary, Monachesi, Antonela, additional, Trager, Scott C., additional, Lauer, Tod R., additional, Saha, Abhijit, additional, Mighell, Kenneth J., additional, Freedman, Wendy, additional, Dressler, Alan, additional, Grillmair, Carl, additional, and Tolstoy, Eline, additional

Published
2009
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126. An environmental dependence of the physical and structural properties in the Hydra cluster galaxies.

Author

Lima-Dias, Ciria, Monachesi, Antonela, Torres-Flores, Sergio, Cortesi, Arianna, Hernández-Lang, Daniel, Barbosa, Carlos Eduardo, Mendes de Oliveira, Claudia, Olave-Rojas, Daniela, Pallero, Diego, Sampedro, Laura, Molino, Alberto, Herpich, Fabio R, Jaffé, Yara L, Amorín, Ricardo, Chies-Santos, Ana L, Dimauro, Paola, Telles, Eduardo, Lopes, Paulo A A, Alvarez-Candal, Alvaro, and Ferrari, Fabricio

Subjects
*GALAXY clusters, *PHASE space, *STELLAR mass, *VISIBLE spectra, *PHASE diagrams, *STAR formation
Abstract

The nearby Hydra cluster (∼50 Mpc) is an ideal laboratory to understand, in detail, the influence of the environment on the morphology and quenching of galaxies in dense environments. We study the Hydra cluster galaxies in the inner regions (1 R 200) of the cluster using data from the Southern Photometric Local Universe Survey, which uses 12 narrow and broad-band filters in the visible region of the spectrum. We analyse structural (Sérsic index, effective radius) and physical (colours, stellar masses, and star formation rates) properties. Based on this analysis, we find that ∼88 per cent of the Hydra cluster galaxies are quenched. Using the Dressler–Schectman test approach, we also find that the cluster shows possible substructures. Our analysis of the phase-space diagram together with densit y- based spatial clustering algorithm indicates that Hydra shows an additional substructure that appears to be in front of the cluster centre, which is still falling into it. Our results, thus, suggest that the Hydra cluster might not be relaxed. We analyse the median Sérsic index as a function of wavelength and find that for red [(u − r) ≥2.3] and earl y- type galaxies it displays a slight increase towards redder filters (13 and 18 per cent, for red and early type, respectively), whereas for blue + green [(u − r)<2.3] galaxies it remains constant. Late-type galaxies show a small decrease of the median Sérsic index towards redder filters. Also, the Sérsic index of galaxies, and thus their structural properties, do not significantly vary as a function of clustercentric distance and density within the cluster; and this is the case regardless of the filter. [ABSTRACT FROM AUTHOR]

Published
2021
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127. The Stellar Populations of M32

Author

Monachesi, Antonela, Trager, S. C., Lauer, Tod R., Freedman, Wendy, Dressler, Alan, Grillmair, Carl, Mighell, Kenneth, Bruzual, GA, Charlot, S, and Astronomy

Subjects
Physics, education.field_of_study, Stellar population, Metallicity, Population, Astronomy, Astronomy and Astrophysics, Astrophysics, Horizontal branch, galaxies: individual: M32, cD, Red-giant branch, Stars, Space and Planetary Science, Local Group, galaxies: stellar content, Asymptotic giant branch, stars: evolution, galaxies: elliptical and lenticular, education, Red clump
Abstract

We present the deepest colour-magnitude diagram (CMD) of M32 to date, obtained from deep (F435W, F555W) photometry of HST ACS/HRC images. Due to the high resolution of our images, the small photometric errors, and the completeness level of our data we obtain the most detailed resolved photometric study of M32 to date. The CMD of M32 displays a wide colour distribution of red giant branch stars, mainly due to a metallicity spread, a strong red clump and bright asymptotic giant branch stars. The detection of a “blue plume” in M32 indicates the presence of a very young stellar population. There is not a noticeable presence of blue horizontal branch stars, suggesting that an old population with [Fe/H] < −1.5 does not significantly contribute to the light or mass of M32 in our observed fields.

Published
2010

128. The resolved stellar populations of M32

Author

Monachesi, Antonela, Trager, Scott, and Astronomy

Subjects
Elliptische sterrenstelsels, Sterrenstelsels, melkwegstelsel, Pleiaden (astronomie), ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Sterevolutie, Proefschriften (vorm), Nevels (astronomie), Gravitatiegolven, Messier 32, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries)
Published
2011

129. M32

Author

Fiorentino, Giuliana, Monachesi, Antonela, Trager, Scott C., Lauer, Tod R., Saha, Abhijit, Mighell, Kenneth J., Freedman, Wendy, Dressler, Alan, Grillmair, Carl, Tolstoy, Eline, Bruzual, GA, Charlot, S, and Kapteyn Astronomical Institute

Subjects
Physics, education.field_of_study, Stellar population, RR LYRAE STARS, Cepheid variable, Population, Astronomy, Astronomy and Astrophysics, Astrophysics, RR Lyrae variable, Photometry (optics), On board, ADVANCED CAMERA, Space and Planetary Science, Hubble space telescope, PHOTOMETRY, Variable star, education, galaxies: elliptical: stars: variables: RR Lyrae
Abstract

We observed two fields near M32 with the ACS/HRC (Program GO-10572, PI: T. Lauer) on board the Hubble Space Telescope, located at distances of about 1.8' and 5.4' (hereafter F1 and F2, respectively) from the center of M32. To obtain a very detailed and deep color-magnitude diagram (CMD) and to look for short period variability, we obtained time-series imaging of each field in 32-orbit-long exposures using the F435W (B) and F555W (V) filters, spanning a temporal range of 2 days per filter. We focus on our detection of variability on RR Lyrae variable stars, which represents the only way to obtain information about the presence of a very old population (larger than 10 Gyr) in M32 from optical data. Here we present results obtained from the detection of 31 RR Lyrae in these fields: 17 in F1 and 14 in F2. We claim we detected 7+4−3 RR Lyrae variables belonging to M32 in F1 thus indicating the presence of a metal-poor ancient population in M32.

Published
2010

130. Pulsaciones no-radiales, no-adiabáticas en estrellas pre-enanas blancas PG1159

Author

Monachesi, Antonela, Córsico, Alejandro Hugo, and Althaus, Leandro Gabriel

Subjects
Astronomía, Ciencias Astronómicas, pulsaciones estelares, pulsaciones adiabáticas noradiales, estrellas enanas blancas
Abstract

Desde hace algunos años, en nuestro Observatorio se ha comenzado el estudio de las pulsaciones estelares en estrellas enanas blancas. Hasta ahora, todos los cálculos han sido realizados dentro de la aproximación adiabática (Córsico, A. H. 1998, 2003). En esta Tesis nos proponemos generalizar el código de pulsaciones adiabáticas no-radiales desarrollado por Córsico, A. H.(1998), relajando la condición de adiabaticidad, de manera que permita calcular pulsaciones no-radiales, no-adiabáticas de estrellas pre-enanas blancas y enanas blancas. La importancia de relajar la condición de adiabaticidad se debe a que esta aproximación, si bien es útil para predecir con gran exactitud el valor de los períodos de oscilación de un dado modelo estelar, no proporciona información acerca de cuáles, de los infinitos modos posibles que conforman el espectro de pulsación, pueden llegar a alcanzar amplitudes lo suficientemente grandes como para ser observados en estrellas reales. Y esto es lo que pretendemos analizar aquí., Facultad de Ciencias Astronómicas y Geofísicas

Published
2006

131. Characterizing dw1335-29, a recently discovered dwarf satellite of M83.

Author

Carrillo, Andreia, Bell, Eric F., Bailin, Jeremy, Monachesi, Antonela, de Jong, Roelof S., Harmsen, Benjamin, and Slater, Colin T.

Subjects
DWARF stars, GALAXY formation, RED giants, VERY large telescopes, STAR formation
Abstract

The number, distribution and properties of dwarf satellites are crucial probes of the physics of galaxy formation at low masses and the response of satellite galaxies to the tidal and gas dynamical effects of their more massive parent. To make progress, it is necessary to augment and solidify the census of dwarf satellites of galaxies outside the Local Group. Müller et al. presented 16 dwarf galaxy candidates near M83, but lacking reliable distances, it is unclear which candidates are M83 satellites. Using red-giant-branch stars from the HST/GHOSTS survey in conjunction with ground-based images from VLT/VIMOS, we confirm that one of the candidates, dw1335-29 - with a projected distance of 26 kpc from M83 and a distance modulus of (m-M)0=28.5-0.1+0.3- is a satellite of M83. We estimate an absolute magnitude MV = -10.1 ± 0.4, an ellipticity of 0.40-0.22+0.14, a half-light radius of 656-170+121 pc and [Fe/H] = -1.3-0.4+0.3 . Owing to dw1335-29's somewhat irregular shape and possible young stars, we classify this galaxy as a dwarf irregular or transition dwarf. This is curious, as with a projected distance of 26 kpc from M83, dw1335-29 is expected to lack recent star formation. Further study of M83's dwarf population will reveal if star formation in its satellites is commonplace (suggesting a lack of a hot gas envelope for M83 that would quench star formation) or rare (suggesting that dw1335-29 has a larger M83-centric distance, and is fortuitously projected to small radii). [ABSTRACT FROM AUTHOR]

Published
2017
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132. GHOSTS I: A NEW FAINT VERY ISOLATED DWARF GALAXY AT D = 12 ± 2 MpcBased on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.

Author

Monachesi, Antonela, Bell, Eric F., Radburn-Smith, David J., Jong, Roelof S. de, Bailin, Jeremy, Dalcanton, Julianne J., Holwerda, Benne W., Ford, H. Alyson, Streich, David, Vlajić, Marija, and Zucker, Daniel B.

Subjects
*DWARF galaxies, *GALACTIC halos, *STAR clusters, *STELLAR luminosity function, *MILKY Way
Abstract

We report the discovery of a new faint dwarf galaxy, GHOSTS I, using HST/ACS data from one of our GHOSTS (Galaxy Halos, Outer disks, Substructure, Thick disk, and Star clusters) fields. Its detected individual stars populate an approximately 1 mag range of its luminosity function (LF). Using synthetic color-magnitude diagrams (CMDs) to compare with the galaxy's CMD, we find that the colors and magnitudes of GHOSTS I's individual stars are most consistent with being young helium-burning and asymptotic giant branch stars at a distance of ∼12 ± 2 Mpc. Morphologically, GHOSTS I appears to be actively forming stars, so we tentatively classify it as a dwarf irregular (dIrr) galaxy, although future Hubble Space Telescope (HST) observations deep enough to resolve a larger magnitude range in its LF are required to make a more secure classification. GHOSTS I's absolute magnitude is , making it one of the least luminous dIrr galaxies known, and its metallicity is lower than [Fe/H] = –1.5 dex. The half-light radius of GHOSTS I is 226 ± 38 pc and its ellipticity is 0.47 ± 0.07, similar to Milky Way and M31 dwarf satellites at comparable luminosity. There are no luminous massive galaxies or galaxy clusters within ∼4 Mpc from GHOSTS I that could be considered as its host, making it a very isolated dwarf galaxy in the local universe. [ABSTRACT FROM AUTHOR]

Published
2014
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133. CONSTRAINING THE AGE OF THE NGC 4565 H I DISK WARP: DETERMINING THE ORIGIN OF GAS WARPS.

Author

Radburn-Smith, David J., Jong, Roelof S. de, Streich, David, Bell, Eric F., Dalcanton, Julianne J., Dolphin, Andrew E., Stilp, Adrienne M., Monachesi, Antonela, Holwerda, Benne W., and Bailin, Jeremy

Subjects
GALAXY formation, DISTRIBUTION of stars, SPIRAL galaxies, DISKS (Astrophysics), ASYMPTOTIC giant branch stars
Abstract

We have mapped the distribution of young and old stars in the gaseous H I warp of NGC 4565. We find a clear correlation of young stars (<600 Myr) with the warp but no coincident old stars (>1 Gyr), which places an upper limit on the age of the structure. The formation rate of the young stars, which increased ∼300 Myr ago relative to the surrounding regions, is M☼ yr–1 kpc–2. This implies a ∼60 ± 20 Gyr depletion time of the H I warp, similar to the timescales calculated for the outer H I disks of nearby spiral galaxies. While some stars associated with the warp fall into the asymptotic giant branch (AGB) region of the color-magnitude diagram, where stars could be as old as 1 Gyr, further investigation suggests that they may be interlopers rather than real AGB stars. We discuss the implications of these age constraints for the formation of H I warps and the gas fueling of disk galaxies. [ABSTRACT FROM AUTHOR]

Published
2014
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134. RR LYRAE VARIABLES IN M32 AND THE DISK OF M31

Author

Fiorentino, Giuliana, Monachesi, Antonela, Trager, Scott C., Lauer, Tod R., Saha, Abhijit, Mighell, Kenneth J., Freedman, Wendy, Dressler, Alan, Grillmair, Carl, and Tolstoy, Eline

Abstract

We observed two fields near M32 with the Advanced Camera for Surveys/High Resolution Channel (ACS/HRC) on board the Hubble Space Telescope. The main field, F1, is 1.'8 from the center of M32; the second field, F2, constrains the M31 background, and is 5.'4 distant. Each field was observed for 16 orbits in each of the F435W (narrow B) and F555W (narrow V) filters. The duration of the observations allowed RR Lyrae stars to be detected. A population of RR Lyrae stars determined to belong to M32 would prove the existence of an ancient population in that galaxy, a subject of some debate. We detected 17 RR Lyrae variables in F1 and 14 in F2. A 1s upper limit of 6 RR Lyrae variables belonging to M32 is inferred from these two fields alone. Use of our two ACS/WFC parallel fields provides better constraints on the M31 background, however, and implies that 7+4 -3 (68% confidence interval) RR Lyrae variables in F1 belong to M32. We have therefore found evidence for an ancient population in M32. It seems to be nearly indistinguishable from the ancient population of M31. The RR Lyrae stars in the F1 and F2 fields have indistinguishable mean V-band magnitudes, mean periods, distributions in the Bailey diagram, and ratios of RRc to RRtotal types. However, the color distributions in the two fields are different, with a population of red RRab variables in F1 not seen in F2. We suggest that these might be identified with the detected M32 RR Lyrae population, but the small number of stars rules out a definitive claim.

Published
2010

135. First Results from the Survey of the MAgellanic Stellar History (SMASH)

Author

Nidever, David L., Olsen, Knut A., Gruendl, Robert A., Besla, Gurtina, Saha, Abi, Olszewski, Edward, Munoz, Ricardo, Gallart, Carme, Monelli, Matteo, Walker, Alistair R., Blum, Robert D., Kaleida, Catherine C., Vivas, Kathy, Majewski, Steven R., Zaritsky, Dennis F., Roeland van der Marel, Bell, Eric F., Conn, Blair, Stringfellow, Guy S., Jin, Shoko, Monteagudo Nervion, Lara, Cioni, Maria-Rosa, Noel, Noelia, Martin, Nicolas, Monachesi, Antonela, Boer, Thomas, Chu, You-Hua, Kim, Hwihyun, Martinez-Delgado, David, Johnson, Lent C., Kunder, Andrea, and Smash

136. Survey of the MAgellanic Stellar History -- SMASH

Author

Nidever, David, Olsen, Knut, Besla, Gurtina, Gruendl, Robert, Saha, Abhijit, Gallart, Carme, Olszewski, Edward W., Munoz, Ricardo, Monelli, Matteo, Kunder, Andrea, Kaleida, Catherine, Walker, Alistair, Stringfellow, Guy, Zaritsky, Dennis, Roeland van der Marel, Blum, Robert, Vivas, Kathy, Chu, You-Hua, Martin, Nicolas, Conn, Blair, Noel, Noelia, Majewski, Steven, Jin, Shoko, Kim, Hwihyun, Cioni, Maria-Rosa, Bell, Eric, Monachesi, Antonela, Boer, Thomas, and Kapteyn Astronomical Institute

Abstract

Over the last several years, various discoveries have drastically altered our view of the iconic Magellanic Clouds (MCs), the nearest interacting galaxy system. The best evidence is now that they are on first infall into the Milky Way, that their stellar populations extend much further than previously thought, and that they suffered a close collision that tore out both the well-known Magellanic Stream and a large amount of still undetected stellar debris. Here we propose a community DECam survey of the Clouds mapping 480 deg^2 (distributed over 2400 deg^2 at 20% filling factor) to 24th mag griz (and u$ 23) that will supplement the 5000 deg^2 Dark Energy Survey's partial coverage of the Magellanic periphery, allowing us to map the expected stellar debris and extended populations with unprecedented fidelity. We have already conducted a pilot project demonstrating that DECam will allow us to: (1) Map the stellar periphery of the MCs with old main-sequence turnoff stars to a surface brightness limit of 35 mag/arcsec^2, revealing relics of their formation and past interactions. (2) Identify the stellar component of the Magellanic Stream and Leading Arm for the first time, if they exist, making them the only Galactic halo tracers with both gaseous and stellar components. (3) Derive spatially-resolved star formation histories covering all ages out to large radii of the MCs that will further complement our understanding of their formation. The combination of this survey and DES data will allow us to uncover a multitude of stellar structure that will unveil the complex and dramatic history of these two dwarf galaxies, while enabling a broad spectrum of community-led projects.

138. The Auriga stellar haloes: connecting stellar population properties with accretion and merging history

Author

Antonela Monachesi, Volker Springel, Guinevere Kauffmann, Simon D. M. White, Christine M. Simpson, Patricia B. Tissera, Facundo A. Gómez, Sebastian Bustamante, Federico Marinacci, Rüdiger Pakmor, Carlos S. Frenk, Robert J. J. Grand, Monachesi, Antonela, Gómez, Facundo A, Grand, Robert J J, Simpson, Christine M, Kauffmann, Guinevere, Bustamante, Sebastián, Marinacci, Federico, Pakmor, Rüdiger, Springel, Volker, Frenk, Carlos S, White, Simon D M, and Tissera, Patricia B

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Stellar population, Metallicity, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, AURIGA, 010308 nuclear & particles physics, methods: numerical – galaxies: haloes – galaxies: spiral – galaxies: stellar content, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We examine the stellar haloes of the Auriga simulations, a suite of thirty cosmological magneto-hydrodynamical high-resolution simulations of Milky Way-mass galaxies performed with the moving-mesh code AREPO. We study halo global properties and radial profiles out to $\sim 150$ kpc for each individual galaxy. The Auriga haloes are diverse in their masses and density profiles; mean metallicity and metallicity gradients; ages; and shapes, reflecting the stochasticity inherent in their accretion and merger histories. A comparison with observations of nearby late-type galaxies shows very good agreement between most observed and simulated halo properties. However, Auriga haloes are typically too massive. We find a connection between population gradients and mass assembly history: galaxies with few significant progenitors have more massive haloes, possess large negative halo metallicity gradients and steeper density profiles. The number of accreted galaxies, either disrupted or under disruption, that contribute 90% of the accreted halo mass ranges from 1 to 14, with a median of 6.5, and their stellar masses span over three orders of magnitude. The observed halo mass--metallicity relation is well reproduced by Auriga and is set by the stellar mass and metallicity of the dominant satellite contributors. This relationship is found not only for the accreted component but also for the total (accreted + in-situ) stellar halo. Our results highlight the potential of observable halo properties to infer the assembly history of galaxies., Comment: Accepted to MNRAS. 30 pages, 19 figures

Published
2019

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