@article{GoettgensWeilbacherRothetal.2019, author = {G{\"o}ttgens, Fabian and Weilbacher, Peter Michael and Roth, Martin M. and Dreizler, Stefan and Giesers, Benjamin and Husser, Tim-Oliver and Kamann, Sebastian and Brinchmann, Jarle and Kollatschny, Wolfram and Monreal-Ibero, Ana and Schmidt, Kasper Borello and Wendt, Martin and Wisotzki, Lutz and Bacon, Roland}, title = {Discovery of an old nova remnant in the Galactic globular cluster M 22}, series = {Astronomy and astrophysics : an international weekly journal}, volume = {626}, journal = {Astronomy and astrophysics : an international weekly journal}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {1432-0746}, doi = {10.1051/0004-6361/201935221}, pages = {6}, year = {2019}, abstract = {A nova is a cataclysmic event on the surface of a white dwarf in a binary system that increases the overall brightness by several orders of magnitude. Although binary systems with a white dwarf are expected to be overabundant in globular clusters compared with in the Galaxy, only two novae from Galactic globular clusters have been observed. We present the discovery of an emission nebula in the Galactic globular cluster M 22 (NGC 6656) in observations made with the integral-field spectrograph MUSE. We extracted the spectrum of the nebula and used the radial velocity determined from the emission lines to confirm that the nebula is part of NGC 6656. Emission-line ratios were used to determine the electron temperature and density. It is estimated to have a mass of 1-17 x 10(-5) M-circle dot. This mass and the emission-line ratios indicate that the nebula is a nova remnant. Its position coincides with the reported location of a "guest star", an ancient Chinese term for transients, observed in May 48 BCE. With this discovery, this nova may be one of the oldest confirmed extra-solar events recorded in human history.}, language = {en} } @article{KamannHusserDreizleretal.2017, author = {Kamann, Sebastian and Husser, T. -O. and Dreizler, S. and Emsellem, E. and Weilbacher, Peter Michael and Martens, S. and Bacon, R. and den Brok, M. and Giesers, B. and Krajnovic, Davor and Roth, Martin M. and Wendt, Martin and Wisotzki, Lutz}, title = {A stellar census in globular clusters with MUSE}, series = {Monthly notices of the Royal Astronomical Society}, volume = {473}, journal = {Monthly notices of the Royal Astronomical Society}, number = {4}, publisher = {Oxford Univ. Press}, address = {Oxford}, issn = {0035-8711}, doi = {10.1093/mnras/stx2719}, pages = {5591 -- 5616}, year = {2017}, abstract = {This is the first of a series of papers presenting the results from our survey of 25 Galactic globular clusters with the MUSE integral-field spectrograph. In combination with our dedicated algorithm for source deblending, MUSE provides unique multiplex capabilities in crowded stellar fields and allows us to acquire samples of up to 20 000 stars within the half-light radius of each cluster. The present paper focuses on the analysis of the internal dynamics of 22 out of the 25 clusters, using about 500 000 spectra of 200 000 individual stars. Thanks to the large stellar samples per cluster, we are able to perform a detailed analysis of the central rotation and dispersion fields using both radial profiles and two-dimensional maps. The velocity dispersion profiles we derive show a good general agreement with existing radial velocity studies but typically reach closer to the cluster centres. By comparison with proper motion data, we derive or update the dynamical distance estimates to 14 clusters. Compared to previous dynamical distance estimates for 47 Tuc, our value is in much better agreement with other methods. We further find significant (>3 sigma) rotation in the majority (13/22) of our clusters. Our analysis seems to confirm earlier findings of a link between rotation and the ellipticities of globular clusters. In addition, we find a correlation between the strengths of internal rotation and the relaxation times of the clusters, suggesting that the central rotation fields are relics of the cluster formation that are gradually dissipated via two-body relaxation.}, language = {en} } @article{AartsAndersonAndersonetal.2015, author = {Aarts, Alexander A. and Anderson, Joanna E. and Anderson, Christopher J. and Attridge, Peter R. and Attwood, Angela and Axt, Jordan and Babel, Molly and Bahnik, Stepan and Baranski, Erica and Barnett-Cowan, Michael and Bartmess, Elizabeth and Beer, Jennifer and Bell, Raoul and Bentley, Heather and Beyan, Leah and Binion, Grace and Borsboom, Denny and Bosch, Annick and Bosco, Frank A. and Bowman, Sara D. and Brandt, Mark J. and Braswell, Erin and Brohmer, Hilmar and Brown, Benjamin T. and Brown, Kristina and Bruening, Jovita and Calhoun-Sauls, Ann and Callahan, Shannon P. and Chagnon, Elizabeth and Chandler, Jesse and Chartier, Christopher R. and Cheung, Felix and Christopherson, Cody D. and Cillessen, Linda and Clay, Russ and Cleary, Hayley and Cloud, Mark D. and Cohn, Michael and Cohoon, Johanna and Columbus, Simon and Cordes, Andreas and Costantini, Giulio and Alvarez, Leslie D. Cramblet and Cremata, Ed and Crusius, Jan and DeCoster, Jamie and DeGaetano, Michelle A. and Della Penna, Nicolas and den Bezemer, Bobby and Deserno, Marie K. and Devitt, Olivia and Dewitte, Laura and Dobolyi, David G. and Dodson, Geneva T. and Donnellan, M. Brent and Donohue, Ryan and Dore, Rebecca A. and Dorrough, Angela and Dreber, Anna and Dugas, Michelle and Dunn, Elizabeth W. and Easey, Kayleigh and Eboigbe, Sylvia and Eggleston, Casey and Embley, Jo and Epskamp, Sacha and Errington, Timothy M. and Estel, Vivien and Farach, Frank J. and Feather, Jenelle and Fedor, Anna and Fernandez-Castilla, Belen and Fiedler, Susann and Field, James G. and Fitneva, Stanka A. and Flagan, Taru and Forest, Amanda L. and Forsell, Eskil and Foster, Joshua D. and Frank, Michael C. and Frazier, Rebecca S. and Fuchs, Heather and Gable, Philip and Galak, Jeff and Galliani, Elisa Maria and Gampa, Anup and Garcia, Sara and Gazarian, Douglas and Gilbert, Elizabeth and Giner-Sorolla, Roger and Gl{\"o}ckner, Andreas and G{\"o}llner, Lars and Goh, Jin X. and Goldberg, Rebecca and Goodbourn, Patrick T. and Gordon-McKeon, Shauna and Gorges, Bryan and Gorges, Jessie and Goss, Justin and Graham, Jesse and Grange, James A. and Gray, Jeremy and Hartgerink, Chris and Hartshorne, Joshua and Hasselman, Fred and Hayes, Timothy and Heikensten, Emma and Henninger, Felix and Hodsoll, John and Holubar, Taylor and Hoogendoorn, Gea and Humphries, Denise J. and Hung, Cathy O. -Y. and Immelman, Nathali and Irsik, Vanessa C. and Jahn, Georg and Jaekel, Frank and Jekel, Marc and Johannesson, Magnus and Johnson, Larissa G. and Johnson, David J. and Johnson, Kate M. and Johnston, William J. and Jonas, Kai and Joy-Gaba, Jennifer A. and Kappes, Heather Barry and Kelso, Kim and Kidwell, Mallory C. and Kim, Seung Kyung and Kirkhart, Matthew and Kleinberg, Bennett and Knezevic, Goran and Kolorz, Franziska Maria and Kossakowski, Jolanda J. and Krause, Robert Wilhelm and Krijnen, Job and Kuhlmann, Tim and Kunkels, Yoram K. and Kyc, Megan M. and Lai, Calvin K. and Laique, Aamir and Lakens, Daniel and Lane, Kristin A. and Lassetter, Bethany and Lazarevic, Ljiljana B. and LeBel, Etienne P. and Lee, Key Jung and Lee, Minha and Lemm, Kristi and Levitan, Carmel A. and Lewis, Melissa and Lin, Lin and Lin, Stephanie and Lippold, Matthias and Loureiro, Darren and Luteijn, Ilse and Mackinnon, Sean and Mainard, Heather N. and Marigold, Denise C. and Martin, Daniel P. and Martinez, Tylar and Masicampo, E. J. and Matacotta, Josh and Mathur, Maya and May, Michael and Mechin, Nicole and Mehta, Pranjal and Meixner, Johannes and Melinger, Alissa and Miller, Jeremy K. and Miller, Mallorie and Moore, Katherine and M{\"o}schl, Marcus and Motyl, Matt and M{\"u}ller, Stephanie M. and Munafo, Marcus and Neijenhuijs, Koen I. and Nervi, Taylor and Nicolas, Gandalf and Nilsonne, Gustav and Nosek, Brian A. and Nuijten, Michele B. and Olsson, Catherine and Osborne, Colleen and Ostkamp, Lutz and Pavel, Misha and Penton-Voak, Ian S. and Perna, Olivia and Pernet, Cyril and Perugini, Marco and Pipitone, R. Nathan and Pitts, Michael and Plessow, Franziska and Prenoveau, Jason M. and Rahal, Rima-Maria and Ratliff, Kate A. and Reinhard, David and Renkewitz, Frank and Ricker, Ashley A. and Rigney, Anastasia and Rivers, Andrew M. and Roebke, Mark and Rutchick, Abraham M. and Ryan, Robert S. and Sahin, Onur and Saide, Anondah and Sandstrom, Gillian M. and Santos, David and Saxe, Rebecca and Schlegelmilch, Rene and Schmidt, Kathleen and Scholz, Sabine and Seibel, Larissa and Selterman, Dylan Faulkner and Shaki, Samuel and Simpson, William B. and Sinclair, H. Colleen and Skorinko, Jeanine L. M. and Slowik, Agnieszka and Snyder, Joel S. and Soderberg, Courtney and Sonnleitner, Carina and Spencer, Nick and Spies, Jeffrey R. and Steegen, Sara and Stieger, Stefan and Strohminger, Nina and Sullivan, Gavin B. and Talhelm, Thomas and Tapia, Megan and te Dorsthorst, Anniek and Thomae, Manuela and Thomas, Sarah L. and Tio, Pia and Traets, Frits and Tsang, Steve and Tuerlinckx, Francis and Turchan, Paul and Valasek, Milan and Van Aert, Robbie and van Assen, Marcel and van Bork, Riet and van de Ven, Mathijs and van den Bergh, Don and van der Hulst, Marije and van Dooren, Roel and van Doorn, Johnny and van Renswoude, Daan R. and van Rijn, Hedderik and Vanpaemel, Wolf and Echeverria, Alejandro Vasquez and Vazquez, Melissa and Velez, Natalia and Vermue, Marieke and Verschoor, Mark and Vianello, Michelangelo and Voracek, Martin and Vuu, Gina and Wagenmakers, Eric-Jan and Weerdmeester, Joanneke and Welsh, Ashlee and Westgate, Erin C. and Wissink, Joeri and Wood, Michael and Woods, Andy and Wright, Emily and Wu, Sining and Zeelenberg, Marcel and Zuni, Kellylynn}, title = {Estimating the reproducibility of psychological science}, series = {Science}, volume = {349}, journal = {Science}, number = {6251}, publisher = {American Assoc. for the Advancement of Science}, address = {Washington}, organization = {Open Sci Collaboration}, issn = {1095-9203}, doi = {10.1126/science.aac4716}, pages = {8}, year = {2015}, abstract = {Reproducibility is a defining feature of science, but the extent to which it characterizes current research is unknown. We conducted replications of 100 experimental and correlational studies published in three psychology journals using high-powered designs and original materials when available. Replication effects were half the magnitude of original effects, representing a substantial decline. Ninety-seven percent of original studies had statistically significant results. Thirty-six percent of replications had statistically significant results; 47\% of original effect sizes were in the 95\% confidence interval of the replication effect size; 39\% of effects were subjectively rated to have replicated the original result; and if no bias in original results is assumed, combining original and replication results left 68\% with statistically significant effects. Correlational tests suggest that replication success was better predicted by the strength of original evidence than by characteristics of the original and replication teams.}, language = {en} } @article{WeilbacherMonrealIberoVerhammeetal.2018, author = {Weilbacher, Peter Michael and Monreal-Ibero, Ana and Verhamme, Anne and Sandin, Christer and Steinmetz, Matthias and Kollatschny, Wolfram and Krajnovic, Davor and Kamann, Sebastian and Roth, Martin M. and Erroz-Ferrer, Santiago and Marino, Raffaella Anna and Maseda, Michael V. and Wendt, Martin and Bacon, Roland and Dreizler, Stefan and Richard, Johan and Wisotzki, Lutz}, title = {Lyman-continuum leakage as dominant source of diffuse ionized gas in the Antennae galaxy}, series = {Astronomy and astrophysics : an international weekly journal}, volume = {611}, journal = {Astronomy and astrophysics : an international weekly journal}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {1432-0746}, doi = {10.1051/0004-6361/201731669}, pages = {17}, year = {2018}, abstract = {The Antennae galaxy (NGC 4038/39) is the closest major interacting galaxy system and is therefore often studied as a merger prototype. We present the first comprehensive integral field spectroscopic dataset of this system, observed with the MUSE instrument at the ESO VLT. We cover the two regions in this system which exhibit recent star formation: the central galaxy interaction and a region near the tip of the southern tidal tail. In these fields, we detect H II regions and diffuse ionized gas to unprecedented depth. About 15\% of the ionized gas was undetected by previous observing campaigns. This newly detected faint ionized gas is visible everywhere around the central merger, and shows filamentary structure. We estimate diffuse gas fractions of about 60\% in the central field and 10\% in the southern region. We are able to show that the southern region contains a significantly different population of H II regions, showing fainter luminosities. By comparing H II region luminosities with the HST catalog of young star clusters in the central field, we estimate that there is enough Lyman-continuum leakage in the merger to explain the amount of diffuse ionized gas that we detect. We compare the Lyman-continuum escape fraction of each H II region against emission line ratios that are sensitive to the ionization parameter. While we find no systematic trend between these properties, the most extreme line ratios seem to be strong indicators of density bounded ionization. Extrapolating the Lyman-continuum escape fractions to the southern region, we conclude that simply from the comparison of the young stellar populations to the ionized gas there is no need to invoke other ionization mechanisms than Lyman-continuum leaking H II regions for the diffuse ionized gas in the Antennae.}, language = {en} } @article{BoucheFinleySchroetteretal.2016, author = {Bouche, Nicolas and Finley, H. and Schroetter, I. and Murphy, M. T. and Richter, Philipp and Bacon, Roland and Contini, Thierry and Richard, J. and Wendt, Martin and Kamann, S. and Epinat, Benoit and Cantalupo, Sebastiano and Straka, Lorrie A. and Schaye, Joop and Martin, C. L. and Peroux, C. and Wisotzki, Lutz and Soto, K. and Lilly, S. and Carollo, C. M. and Brinchmann, Jarle and Kollatschny, W.}, title = {POSSIBLE SIGNATURES OF A COLD-FLOW DISK FROM MUSE USING A z similar to 1 GALAXY-QUASAR PAIR TOWARD SDSS J1422-0001}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, volume = {820}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {0004-637X}, doi = {10.3847/0004-637X/820/2/121}, pages = {1872 -- 1882}, year = {2016}, abstract = {We use a background quasar to detect the presence of circumgalactic gas around a z = 0.91 low-mass star-forming galaxy. Data from the new Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope show that the galaxy has a dust-corrected star formation rate (SFR) of 4.7 +/- 2.0. M-circle dot yr(-1), with no companion down to 0.22 M-circle dot yr(-1) (5 sigma) within 240 h(-1) kpc ("30"). Using a high-resolution spectrum of the background quasar, which is fortuitously aligned with the galaxy major axis (with an azimuth angle alpha of only 15 degrees), we find, in the gas kinematics traced by low-ionization lines, distinct signatures consistent with those expected for a "cold-flow disk" extending at least 12 kpc (3 x R-1/2). We estimate the mass accretion rate M-in to be at least two to three times larger than the SFR, using the geometric constraints from the IFU data and the H (I) column density of log N-H (I)/cm(-2) similar or equal to 20.4 obtained from a Hubble Space Telescope/COS near-UV spectrum. From a detailed analysis of the low-ionization lines (e.g., Zn II, Cr II, Ti II, MnII, Si II), the accreting material appears to be enriched to about 0.4 Z(circle dot) (albeit with large uncertainties: log Z/Z(circle dot) = -0.4 +/- 0.4), which is comparable to the galaxy metallicity (12 + log O/H = 8.7 +/- 0.2), implying a large recycling fraction from past outflows. Blueshifted Mg II and Fe II absorptions in the galaxy spectrum from the MUSE data reveal the presence of an outflow. The Mg II and Fe II absorption line ratios indicate emission infilling due to scattering processes, but the MUSE data do not show any signs of fluorescent Fe II* emission.}, language = {en} } @article{HusserKamannDreizleretal.2016, author = {Husser, Tim-Oliver and Kamann, Sebastian and Dreizler, Stefan and Wendt, Martin and Wulff, Nina and Bacon, Roland and Wisotzki, Lutz and Brinchmann, Jarle and Weilbacher, Peter Michael and Roth, Martin M. and Monreal-Ibero, Ana}, title = {MUSE crowded field 3D spectroscopy of over 12 000 stars in the globular cluster NGC 6397 I. The first comprehensive HRD of a globular cluster}, series = {Nucleic acids research}, volume = {588}, journal = {Nucleic acids research}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {1432-0746}, doi = {10.1051/0004-6361/201526949}, pages = {14}, year = {2016}, abstract = {Aims. We demonstrate the high multiplex advantage of crowded field 3D spectroscopy with the new integral field spectrograph MUSE by means of a spectroscopic analysis of more than 12 000 individual stars in the globular cluster NGC 6397. Methods. The stars are deblended with a point spread function fitting technique, using a photometric reference catalogue from HST as prior, including relative positions and brightnesses. This catalogue is also used for a first analysis of the extracted spectra, followed by an automatic in-depth analysis via a full-spectrum fitting method based on a large grid of PHOENIX spectra. Results. We analysed the largest sample so far available for a single globular cluster of 18 932 spectra from 12 307 stars in NGC 6397. We derived a mean radial velocity of v(rad) = 17.84 +/- 0.07 km s(-1) and a mean metallicity of [Fe/H] = -2.120 +/- 0.002, with the latter seemingly varying with temperature for stars on the red giant branch (RGB). We determine Teff and [Fe/H] from the spectra, and log g from HST photometry. This is the first very comprehensive Hertzsprung-Russell diagram (HRD) for a globular cluster based on the analysis of several thousands of stellar spectra, ranging from the main sequence to the tip of the RGB. Furthermore, two interesting objects were identified; one is a post-AGB star and the other is a possible millisecond-pulsar companion.}, language = {en} } @article{HerderUtechtManickeetal.2013, author = {Herder, Martin and Utecht, Manuel Martin and Manicke, Nicole and Grubert, Lutz and P{\"a}tzel, Michael and Saalfrank, Peter and Hecht, Stefan}, title = {Switching with orthogonal stimuli electrochemical ring-closure and photochemical ring-opening of bis(thiazolyl) maleimides}, series = {Chemical science}, volume = {4}, journal = {Chemical science}, number = {3}, publisher = {Royal Society of Chemistry}, address = {Cambridge}, issn = {2041-6520}, doi = {10.1039/c2sc21681g}, pages = {1028 -- 1040}, year = {2013}, abstract = {The photochemistry as well as electrochemistry of novel donor-acceptor bis(morpholinothiazolyl)maleimides has been investigated. Proper substitution of these diarylethene-type molecular switches leads to the unique situation in which their ring-closure can only be accomplished electrochemically, while ring-opening can only be achieved photochemically. Hence, these switches operate with orthogonal stimuli, i.e. redox potential and light, respectively. The switch system could be optimized by introducing trifluoromethyl groups at the reactive carbon atoms in order to avoid by-product formation during oxidative ring closure. Both photochemical and electrochemical pathways were investigated for methylated, trifluoromethylated, and nonsymmetrical bis(morpholinothiazolyl) maleimides as well as the bis(morpholinothiazolyl) cyclopentene reference compound. With the aid of the nonsymmetrical "mixed" derivative, the mechanism of electrochemically driven ring closure could be elucidated and seems to proceed via a dicationic intermediate generated by two-fold oxidation. All experimental work has been complemented by density functional theory that provides detailed insights into the thermodynamics of the ring-open and closed forms, the nature of their excited states, and the reactivity of their neutral as well as ionized species in different electronic configurations. The particular diarylethene systems described herein could serve in multifunctional (logic) devices operated by different stimuli (inputs) and may pave the way to converting light into electrical energy via photoinduced "pumping" of redox-active meta-stable states.}, language = {en} } @article{BehrensGubeChaabeneetal.2022, author = {Behrens, Martin and Gube, Martin and Chaabene, Helmi and Prieske, Olaf and Zenon, Alexandre and Broscheid, Kim-Charline and Schega, Lutz and Husmann, Florian and Weippert, Matthias}, title = {Fatigue and human performance}, series = {Sports medicine : an international journal of applied medicine and science in sport and exercise}, volume = {53}, journal = {Sports medicine : an international journal of applied medicine and science in sport and exercise}, number = {1}, publisher = {Springer}, address = {Heidelberg}, issn = {0112-1642}, doi = {10.1007/s40279-022-01748-2}, pages = {7 -- 31}, year = {2022}, abstract = {Fatigue has been defined differently in the literature depending on the field of research. The inconsistent use of the term fatigue complicated scientific communication, thereby limiting progress towards a more in-depth understanding of the phenomenon. Therefore, Enoka and Duchateau (Med Sci Sports Exerc 48:2228-38, 2016, [3]) proposed a fatigue framework that distinguishes between trait fatigue (i.e., fatigue experienced by an individual over a longer period of time) and motor or cognitive task-induced state fatigue (i.e., self-reported disabling symptom derived from the two interdependent attributes performance fatigability and perceived fatigability). Thereby, performance fatigability describes a decrease in an objective performance measure, while perceived fatigability refers to the sensations that regulate the integrity of the performer. Although this framework served as a good starting point to unravel the psychophysiology of fatigue, several important aspects were not included and the interdependence of the mechanisms driving performance fatigability and perceived fatigability were not comprehensively discussed. Therefore, the present narrative review aimed to (1) update the fatigue framework suggested by Enoka and Duchateau (Med Sci Sports Exerc 48:2228-38, 2016, [3]) pertaining the taxonomy (i.e., cognitive performance fatigue and perceived cognitive fatigue were added) and important determinants that were not considered previously (e.g., effort perception, affective valence, self-regulation), (2) discuss the mechanisms underlying performance fatigue and perceived fatigue in response to motor and cognitive tasks as well as their interdependence, and (3) provide recommendations for future research on these interactions. We propose to define motor or cognitive task-induced state fatigue as a psychophysiological condition characterized by a decrease in motor or cognitive performance (i.e., motor or cognitive performance fatigue, respectively) and/or an increased perception of fatigue (i.e., perceived motor or cognitive fatigue). These dimensions are interdependent, hinge on different determinants, and depend on body homeostasis (e.g., wakefulness, core temperature) as well as several modulating factors (e.g., age, sex, diseases, characteristics of the motor or cognitive task). Consequently, there is no single factor primarily determining performance fatigue and perceived fatigue in response to motor or cognitive tasks. Instead, the relative weight of each determinant and their interaction are modulated by several factors.}, language = {en} } @article{SchroetterBoucheZabletal.2019, author = {Schroetter, Ilane and Bouche, Nicolas F. and Zabl, Johannes and Contini, Thierry and Wendt, Martin and Schaye, Joop and Mitchell, Peter and Muzahid, Sowgat and Marino, Raffaella Anna and Bacon, Roland and Lilly, Simon J. and Richard, Johan and Wisotzki, Lutz}, title = {MusE GAs FLOw andWind (MEGAFLOW)}, series = {Monthly notices of the Royal Astronomical Society}, volume = {490}, journal = {Monthly notices of the Royal Astronomical Society}, number = {3}, publisher = {Oxford Univ. Press}, address = {Oxford}, issn = {0035-8711}, doi = {10.1093/mnras/stz2822}, pages = {4368 -- 4381}, year = {2019}, abstract = {We present results from our on-going MusE GAs FLOw and Wind (MEGAFLOW) survey, which consists of 22 quasar lines of sight, each observed with the integral field unit MUSE and the UVES spectrograph at the ESO Very Large Telescopes (VLT). The goals of this survey are to study the properties of the circumgalactic medium around z similar to 1 star-forming galaxies. The absorption-line selected survey consists of 79 strong MgII absorbers (with rest-frame equivalent width greater than or similar to 0.3 angstrom) and, currently, 86 associated galaxies within 100 projected kpc of the quasar with stellar masses (M-star) from 109 to 1011 M-circle dot. We find that the cool halo gas traced by MgII is not isotropically distributed around these galaxies from the strong bi-modal distribution in the azimuthal angle of the apparent location of the quasar with respect to the galaxy major axis. This supports a scenario in which outflows are bi-conical in nature and co-exist with a co-planar gaseous structure extending at least up to 60-80 kpc. Assuming that absorbers near the minor axis probe outflows, the current MEGAFLOW sample allowed us to select 26 galaxy-quasar pairs suitable for studying winds. From this sample, using a simple geometrical model, we find that the outflow velocity only exceeds the escape velocity when M-star less than or similar to 4 x 10(9) M-circle dot, implying the cool material is likely to fall back except in the smallest haloes. Finally, we find that the mass loading factor., the ratio between the ejected mass rate and the star formation rate, appears to be roughly constant with respect to the galaxy mass.}, language = {en} } @article{ChristensenSchulteLadbeckSanchezetal.2005, author = {Christensen, Lise Bech and Schulte-Ladbeck, R. E. and Sanchez, Sebastian F. and Becker, Thomas and Jahnke, Knud and Kelz, A. and Roth, Martin M. and Wisotzki, Lutz}, title = {Abundances and kinematics of a candidate sub-damped Lymana galaxy toward PHL 1226}, year = {2005}, abstract = {The spectrum of the quasar PHL 1226 is known to have a strong Mg II and sub-damped Lymanalpha (sub-DLA) absorption line system with N(H I) = (5 +/- 2) x 10(19) cm(-2) at z = 0.1602. Using integral field spectra from the Potsdam Multi Aperture Spectrophotometer (PMAS) we investigate a galaxy at an impact parameter of 6".4 which is most probably responsible for the absorption lines. A fainter galaxy at a similar redshift and a slightly larger distance from the QSO is known to exist, but we assume that the absorption is caused by the more nearby galaxy. From optical Balmer lines we estimate an intrinsic reddening consistent with 0, and a moderate star formation rate of 0.5 M-circle dot yr(-1) is inferred from the Ha luminosity. Using nebular emission line ratios we find a solar oxygen abundance 12 + log (O/H) = 8.7 +/- 0.1 and a solar nitrogen to oxygen abundance ratio log (N/O) = -1.0 +/- 0.2. This abundance is larger than those of all known sub-DLA systems derived from analyses of metal absorption lines in quasar spectra. On the other hand, the properties are compatible with the most metal rich galaxies responsible for strong Mg II absorption systems. These two categories can be reconciled if we assume an abundance gradient similar to local galaxies. Under that assumption we predict abundances 12 + log (O/H) = 7.1 and log (N/O) = -1.9 for the sub-DLA cloud, which is similar to high redshift DLA and sub-DLA systems. We find evidence for a rotational velocity of similar to200 km s(-1) over a length of similar to7 kpc. From the geometry and kinematics of the galaxy we estimate that the absorbing cloud does not belong to a rotating disk, but could originate in a rotating halo}, language = {en} }