TY  - JOUR
A1  - Wendt, Martin
A1  - Bouche, Nicolas F.
A1  - Zabl, Johannes
A1  - Schroetter, Ilane
A1  - Muzahid, Sowgat
T1  - MusE GAs FLOw and Wind V. The dust/metallicity-anisotropy of the circum-galactic medium
JF  - Monthly notices of the Royal Astronomical Society
N2  - We investigate whether the dust content of the circum-galactic medium (CGM) depends on the location of the quasar sightline with respect to the galaxy major-axis using 13 galaxy-Mg II absorber pairs (9-81 kpc distance) from the MusE GAs FLOw and Wind (MEGAFLOW) survey at 0.4 < z < 1.4. The dust content of the CGM is obtained from [Zn/Fe] using ultraviolet and visual echelle spectrograph data. When a direct measurement of [Zn/Fe] is unavailable, we estimate the dust depletion from a method that consists in solving for the depletion from multiple singly ionized ions (e.g. Mn II, Cr II, and Zn II) since each ion depletes on dust grains at different rates. We find a positive correlation between the azimuthal angle and [Zn/Fe] with a Pearson's gamma = 0.70 +/- 0.14. The sightlines along the major axis show [Zn/Fe] < 0.5, whereas the [Zn/Fe] is > 0.8 along the minor axis. These results suggest that the CGM along the minor axis is on average more metal enriched (by approximate to 1 dex) than the gas located along the major axis of galaxies provided that dust depletion is a proxy for metallicity. This anisotropic distribution is consistent with recent results on outflow and accretion in hydro-dynamical simulations.
KW  - galaxies: evolution
KW  - galaxies: formation
KW  - intergalactic medium
KW  - quasars:
KW  - absorption lines
Y1  - 2021
U6  - https://doi.org/10.1093/mnras/stab049
SN  - 0035-8711
SN  - 1365-2966
VL  - 502
IS  - 3
SP  - 3733
EP  - 3745
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Tomas, Sara
A1  - Homann, Martin
A1  - Mutti, Maria
A1  - Amour, Frederic
A1  - Christ, Nicolas
A1  - Immenhauser, Adrian
A1  - Agar, Susan M.
A1  - Kabiri, Lahcen
T1  - Alternation of microbial mounds and ooid shoals (Middle Jurasssic, Morocco) - response to paleoenvironmental changes
JF  - Sedimentary geology : international journal of applied and regional sedimentology
N2  - The occurrence of neritic microbial carbonates is often related to ecological refuges, where grazers and other competitors are reduced by environmental conditions, or to post-extinction events (e.g. in the Late Devonian, Early Triassic). Here, we present evidence for Middle Jurassic (Bajocian) microbial mounds formed in the normal marine, shallow neritic setting of an inner, ramp system from the High Atlas of Morocco. The microbial mounds are embedded in cross-bedded oolitic facies. Individual mounds show low relief domal geometries (up to 3 m high and 4.5 m across), but occasionally a second generation of mounds exhibits tabular geometries (<1 m high). The domes are circular in plan view and have intact tops, lacking evidence of current influence on mound preferred growth direction or distribution patterns, or truncation. The mound fades consists almost entirely of non-laminated, micritic thrombolites with branching morphologies and fine-grained, clotted and peloidal fabrics. Normal marine biota are present but infrequent. Several lines of evidence document that microbial mound growth alternates with time intervals of active ooid shoal deposition. This notion is of general significance when compared with modern Bahamian microbialites that co-exist with active sub-aquatic dunes. Furthermore, the lack of detailed studies of Middle Jurassic, normal marine shallow neritic microbial mounds adds a strong motivation for the present study. Specifically, Bajocian mounds formed on a firmground substratum during transgressive phases under condensed sedimentation. Furthermore, a transient increase in nutrient supply in the prevailing mesotrophic setting, as suggested by the heterotrophic-dominated biota, may have controlled microbial mound stages.
KW  - Microbial mounds
KW  - Thrombolites
KW  - Ooid shoals
KW  - Paleoenvironment
KW  - Jurassic
Y1  - 2013
U6  - https://doi.org/10.1016/j.sedgeo.2013.05.008
SN  - 0037-0738
VL  - 294
SP  - 68
EP  - 82
PB  - Elsevier
CY  - Amsterdam
ER  - 
TY  - JOUR
A1  - Schroetter, I.
A1  - Bouche, Nicolas
A1  - Wendt, Martin
A1  - Contini, Thierry
A1  - Finley, H.
A1  - Pello, R.
A1  - Bacon, Roland
A1  - Cantalupo, Sebastiano
A1  - Marino, Raffaella Anna
A1  - Richard, J.
A1  - Lilly, S. J.
A1  - Schaye, Joop
A1  - Soto, K.
A1  - Steinmetz, Matthias
A1  - Straka, Lorrie A.
A1  - Wisotzki, Lutz
T1  - MUSE GAS FLOW AND WIND (MEGAFLOW). I. FIRST MUSE RESULTS ON BACKGROUND QUASARS
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2  - The physical properties of galactic winds are one of the keys to understand galaxy formation and evolution. These properties can be constrained thanks to background quasar lines of sight (LOS) passing near star-forming galaxies (SFGs). We present the first results of the MusE GAs FLOw and Wind survey obtained from two quasar fields, which have eight Mg II absorbers of which three have rest equivalent width greater than 0.8 angstrom. With the new Multi Unit Spectroscopic Explorer (MUSE) spectrograph on the Very Large Telescope (VLT), we detect six (75%) Mg II host galaxy candidates within a radius of 30. from the quasar LOS. Out of these six galaxy-quasar pairs, from geometrical argument, one is likely probing galactic outflows, where two are classified as "ambiguous,"two are likely probing extended gaseous disks and one pair seems to be a merger. We focus on the wind-pair and constrain the outflow using a high-resolution quasar spectra from the Ultraviolet and Visual Echelle Spectrograph. Assuming the metal absorption to be due to ga;s flowing out of the detected galaxy through a cone along the minor axis, we find outflow velocities in the order of approximate to 150 km s(-1) (i.e., smaller than the escape velocity) with a loading factor, eta = M-out/SFR, of approximate to 0.7. We see evidence for an open conical flow, with a low-density inner core. In the future, MUSE will provide us with about 80 multiple galaxy-quasar pairs in two dozen fields.
KW  - galaxies: evolution
KW  - galaxies: formation
KW  - intergalactic medium
KW  - quasars: individual (SDSS J213748+001220, SDSS J215200+062516)
Y1  - 2016
U6  - https://doi.org/10.3847/1538-4357/833/1/39
SN  - 0004-637X
SN  - 1538-4357
VL  - 833
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Douglas, John
A1  - Akkar, Sinan
A1  - Ameri, Gabriele
A1  - Bard, Pierre-Yves
A1  - Bindi, Dino
A1  - Bommer, Julian J.
A1  - Bora, Sanjay Singh
A1  - Cotton, Fabrice
A1  - Derras, Boumediene
A1  - Hermkes, Marcel
A1  - Kuehn, Nicolas Martin
A1  - Luzi, Lucia
A1  - Massa, Marco
A1  - Pacor, Francesca
A1  - Riggelsen, Carsten
A1  - Sandikkaya, M. Abdullah
A1  - Scherbaum, Frank
A1  - Stafford, Peter J.
A1  - Traversa, Paola
T1  - Comparisons among the five ground-motion models developed using RESORCE for the prediction of response spectral accelerations due to earthquakes in Europe and the Middle East
JF  - Bulletin of earthquake engineering : official publication of the European Association for Earthquake Engineering
N2  - This article presents comparisons among the five ground-motion models described in other articles within this special issue, in terms of data selection criteria, characteristics of the models and predicted peak ground and response spectral accelerations. Comparisons are also made with predictions from the Next Generation Attenuation (NGA) models to which the models presented here have similarities (e.g. a common master database has been used) but also differences (e.g. some models in this issue are nonparametric). As a result of the differing data selection criteria and derivation techniques the predicted median ground motions show considerable differences (up to a factor of two for certain scenarios), particularly for magnitudes and distances close to or beyond the range of the available observations. The predicted influence of style-of-faulting shows much variation among models whereas site amplification factors are more similar, with peak amplification at around 1s. These differences are greater than those among predictions from the NGA models. The models for aleatory variability (sigma), however, are similar and suggest that ground-motion variability from this region is slightly higher than that predicted by the NGA models, based primarily on data from California and Taiwan.
KW  - Strong-motion data
KW  - Ground-motion models
KW  - Ground-motion prediction equations
KW  - Style of faulting
KW  - Site amplification
KW  - Aleatory variability
KW  - Epistemic uncertainty
KW  - Europe
KW  - Middle East
Y1  - 2014
U6  - https://doi.org/10.1007/s10518-013-9522-8
SN  - 1570-761X
SN  - 1573-1456
VL  - 12
IS  - 1
SP  - 341
EP  - 358
PB  - Springer
CY  - Dordrecht
ER  - 
TY  - JOUR
A1  - Martin, Nicolas F.
A1  - Nidever, David L.
A1  - Besla, Gurtina
A1  - Olsen, Knut
A1  - Walker, Alistair R.
A1  - Vivas, A. Katherina
A1  - Gruendl, Robert A.
A1  - Kaleida, Catherine C.
A1  - Munoz, Ricardo R.
A1  - Blum, Robert D.
A1  - Saha, Abhijit
A1  - Conn, Blair C.
A1  - Bell, Eric F.
A1  - Chu, You-Hua
A1  - Cioni, Maria-Rosa L.
A1  - de Boer, Thomas J. L.
A1  - Gallart, Carme
A1  - Jin, Shoko
A1  - Kunder, Andrea
A1  - Majewski, Steven R.
A1  - Martinez-Delgado, David
A1  - Monachesi, Antonela
A1  - Monelli, Matteo
A1  - Monteagudo, Lara
A1  - Noel, Noelia E. D.
A1  - Olszewski, Edward W.
A1  - Stringfellow, Guy S.
A1  - van der Marel, Roeland P.
A1  - Zaritsky, Dennis
T1  - Hydra II: A faint and compact milky way dwarf galaxy found in the survey of the magellanic stellar history
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters
N2  - We present the discovery of a new dwarf galaxy, Hydra II, found serendipitously within the data from the ongoing Survey of the Magellanic Stellar History conducted with the Dark Energy Camera on the Blanco 4 m Telescope. The new satellite is compact (r(h) = 68 +/- 11 pc) and faint (MV = -4.8 +/- 0.3), but well within the realm of dwarf galaxies. The stellar distribution of Hydra II in the color-magnitude diagram is well-described by a metal-poor ([Fe/H] = -2.2) and old (13 Gyr) isochrone and shows a distinct blue horizontal branch, some possible red clump stars, and faint stars that are suggestive of blue stragglers. At a heliocentric distance of 134 +/- 10 kpc, Hydra II is located in a region of the Galactic halo that models have suggested may host material from the leading arm of the Magellanic Stream. A comparison with N-body simulations hints that the new dwarf galaxy could be or could have been a satellite of the Magellanic Clouds.
KW  - galaxies: individual (Hydra II)
KW  - Local Group
KW  - Magellanic Clouds
Y1  - 2015
U6  - https://doi.org/10.1088/2041-8205/804/1/L5
SN  - 2041-8205
SN  - 2041-8213
VL  - 804
IS  - 1
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Martin, Nicolas F.
A1  - Jungbluth, Valentin
A1  - Nidever, David L.
A1  - Bell, Eric F.
A1  - Besla, Gurtina
A1  - Blum, Robert D.
A1  - Cioni, Maria-Rosa L.
A1  - Conn, Blair C.
A1  - Kaleida, Catherine C.
A1  - Gallart, Carme
A1  - Jin, Shoko
A1  - Majewski, Steven R.
A1  - Martinez-Delgado, David
A1  - Monachesi, Antonela
A1  - Munoz, Ricardo R.
A1  - Noel, Noelia E. D.
A1  - Olsen, Knut
A1  - Stringfellow, Guy S.
A1  - van der Marel, Roeland P.
A1  - Vivas, A. Katherina
A1  - Walker, Alistair R.
A1  - Zaritsky, Dennis
T1  - SMASH 1: A VERY FAINT GLOBULAR CLUSTER DISRUPTING IN THE OUTER REACHES OF THE LMC?
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters
KW  - globular clusters: individual: (SMASH 1)
KW  - Local Group
KW  - Magellanic Clouds
Y1  - 2016
U6  - https://doi.org/10.3847/2041-8205/830/1/L10
SN  - 2041-8205
SN  - 2041-8213
VL  - 830
SP  - 92
EP  - 98
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Nidever, David L.
A1  - Olsen, Knut
A1  - Walker, Alistair R.
A1  - Katherina Vivas, A.
A1  - Blum, Robert D.
A1  - Kaleida, Catherine
A1  - Choi, Yumi
A1  - Conn, Blair C.
A1  - Gruendl, Robert A.
A1  - Bell, Eric F.
A1  - Besla, Gurtina
A1  - Munoz, Ricardo R.
A1  - Gallart, Carme
A1  - Martin, Nicolas F.
A1  - Olszewski, Edward W.
A1  - Saha, Abhijit
A1  - Monachesi, Antonela
A1  - Monelli, Matteo
A1  - de Boer, Thomas J. L.
A1  - Johnson, L. Clifton
A1  - Zaritsky, Dennis
A1  - Stringfellow, Guy S.
A1  - van der Marel, Roeland P.
A1  - Cioni, Maria-Rosa L.
A1  - Jin, Shoko
A1  - Majewski, Steven R.
A1  - Martinez-Delgado, David
A1  - Monteagudo, Lara
A1  - Noel, Noelia E. D.
A1  - Bernard, Edouard J.
A1  - Kunder, Andrea
A1  - Chu, You-Hua
A1  - Bell, Cameron P. M.
A1  - Santana, Felipe
A1  - Frechem, Joshua
A1  - Medina, Gustavo E.
A1  - Parkash, Vaishali
A1  - Seron Navarrete, J. C.
A1  - Hayes, Christian
T1  - SMASH: Survey of the MAgellanic Stellar History
JF  - The astronomical journal
N2  - The Large and Small Magellanic Clouds are unique local laboratories for studying the formation and evolution of small galaxies in exquisite detail. The Survey of the MAgellanic Stellar History (SMASH) is an NOAO community Dark Energy Camera (DECam) survey of the Clouds mapping 480 deg2 (distributed over similar to 2400 square degrees at similar to 20% filling factor) to similar to 24th. mag in ugriz. The primary goals of SMASH are to identify low surface brightness stellar populations associated with the stellar halos and tidal debris of the Clouds, and to derive spatially resolved star formation histories. Here, we present a summary of the survey, its data reduction, and a description of the first public Data Release (DR1). The SMASH DECam data have been reduced with a combination of the NOAO Community Pipeline, the PHOTRED automated point-spread-function photometry pipeline, and custom calibration software. The astrometric precision is similar to 15 mas and the accuracy is similar to 2 mas with respect to the Gaia reference frame. The photometric precision is similar to 0.5%-0.7% in griz and similar to 1% in u with a calibration accuracy of similar to 1.3% in all bands. The median 5s point source depths in ugriz are 23.9, 24.8, 24.5, 24.2, and 23.5 mag. The SMASH data have already been used to discover the Hydra II Milky Way satellite, the SMASH 1 old globular cluster likely associated with the LMC, and extended stellar populations around the LMC out to R. similar to. 18.4 kpc. SMASH DR1 contains measurements of similar to 100 million objects distributed in 61 fields. A prototype version of the NOAO Data Lab provides data access and exploration tools.
KW  - galaxies: dwarf
KW  - galaxies: individual (Large Magellanic Cloud, Small Magellanic Cloud)
KW  - Local Group
KW  - Magellanic Clouds
KW  - surveys
Y1  - 2017
U6  - https://doi.org/10.3847/1538-3881/aa8d1c
SN  - 0004-6256
SN  - 1538-3881
VL  - 154
SP  - 310
EP  - 326
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  -