Katharina Lutz

Université de Strasbourg

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Barbara Catinella

International Centre for Radio Astronomy Research

V. A. Kilborn

Swinburne University of Technology

Helga Dénes

Universidad Yachay Tech

B. Koribalski

Australia Telescope National Facility

O. I. Wong

University of Western Australia

L. Cortese

University of Western Australia

Danail Obreschkow

International Centre for Radio Astronomy Research

G. I. G. Józsa

Rhodes University

R. Genzel

Max Planck Institute for Extraterrestrial Physics

C. Krämer

Institut de Radioastronomie Millimétrique

Cooperative Institutions

ASTRO-3D

ARC Centre of Excellence for All-sky Astrophysics

International Centre for Radio Astronomy Research

University of Western Australia

Max Planck Institute for Extraterrestrial Physics

Commonwealth Scientific and Industrial Research Organisation

Astronomy and Space

Max Planck Society

Swinburne University of Technology

Australian National University

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The HIX galaxy survey I: Study of the most gas rich galaxies from HIPASS

Monthly Notices of the Royal Astronomical Society (2017)

Katharina Lutz V. A. Kilborn Barbara Catinella B. Koribalski Toby Brown

We present the HI eXtreme (HIX) galaxy survey targeting some of the most HI rich galaxies in the southern hemisphere. The 13 HIX galaxies have been selected to host the most massive HI discs at a given stellar luminosity. We compare these galaxies to a control sample of average galaxies detected in the HI Parkes All Sky Survey (HIPASS, Barnes et al. 2001). As the control sample is matched in stellar luminosity, we find that the stellar properties of HIX galaxies are similar to the control sample. Furthermore, the specific star formation rate and optical morphology do not differ between HIX and control galaxies. We find, however, the HIX galaxies to be less efficient in forming stars. For the most HI massive galaxy in our sample (ESO075-G006, $\rm log\ M_{HI}\ [M_{\odot}] = 10.8$) the kinematic properties are the reason for inefficient star formation and HI excess. Examining the Australian Telescope Compact Array (ATCA) HI imaging and Wide Field Spectrograph (WiFeS) optical spectra of ESO075-G006 reveals an undisturbed galaxy without evidence for recent major, violent accretion events. A tilted-ring fit to the HI disc together with the gas-phase oxygen abundance distribution supports the scenario that gas has been constantly accreted onto ESO07-G006 but the high specific angular momentum makes ESO075-G006 very inefficient in forming stars. Thus a massive HI disc has been built up.

10.1093/mnras/stx053

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Citations (22)

Traumatic brain injury in the elderly after a skiing accident: A retrospective cohort study in a level 1 emergency department in Switzerland

PLoS ONE (2022)

Alberto Consuegra Katharina Lutz Aristomenis K. Exadaktylos Werner J. Z’Graggen Rebecca M. Hasler

Background Skiing is a very popular sport worldwide, with increasing trends over the past decades. This study aimed to evaluate the importance of traumatic brain injury (TBI), especially in the elderly, after a ski accident, and to describe its short-term repercussions. Methodology Patients were analyzed who were admitted to our neurotrauma center from 2012–2018 after a head trauma while skiing. Three different age groups were differentiated and analyzed for the severity of TBI depending on the initial Glasgow Coma Scale as the primary outcome and as secondary outcomes need and type of surgery, Glasgow Outcome Score, preexisting use of anticoagulant or antiplatelet drugs, time to presentation, and pattern of brain injury. TBI severity was adjusted to the time to initial medical consultation. Results No significant difference in TBI severity was found when comparing the middle (>29–54) and older (≥54) age groups to the reference group <30 years (OR:0.45, p = 0.127; OR:0.46, p = 0.17). Acute subdural hemorrhage was present in 21.2% of the ≥55 group and 14.5% of the 30–54 age group, compared to 12.8% of the youngest group (p = <0.001). Overall, 39.4% of the patients in the ≥55 group and 8.1% of the 30–54 age group presented with chronic subdural hemorrhage, whereas none of the youngest patients did (p = <0.001). Conclusion No differences were observed in terms of TBI severity between age groups after acute trauma. Nonetheless, a different pattern of head injury after TBI in older patients was demonstrated. Accordingly, the management differs for these TBIs compared to those of younger patients.

Glasgow Outcome Scale

Trauma Center

Head trauma

10.1371/journal.pone.0273168

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Citations (2)

Local Volume TiNy Titans: gaseous dwarf–dwarf interactions in the Local Universe

Monthly Notices of the Royal Astronomical Society (2016)

Sarah Pearson Gurtina Besla M. E. Putman Katharina Lutz Ximena Fernández

In this paper, we introduce the Local Volume TiNy Titans sample (LV-TNT), which is a part of a larger body of work on interacting dwarf galaxies: TNT . This LV-TNT sample consists of 10 dwarf galaxy pairs in the Local Universe (<30 Mpc from Milky Way), which span mass ratios of M*, 1/M*, 2 < 20, projected separations <100 kpc, and pair member masses of log(M*/M⊙) < 9.9. All 10 LV-TNT pairs have resolved synthesis maps of their neutral hydrogen, are located in a range of environments and captured at various interaction stages. This enables us to do a comparative study of the diffuse gas in dwarf–dwarf interactions and disentangle the gas lost due to interactions with haloes of massive galaxies, from the gas lost due to mutual interaction between the dwarfs. We find that the neutral gas is extended in the interacting pairs when compared to non-paired analogues, indicating that gas is tidally pre-processed. Additionally, we find that the environment can shape the H i distributions in the form of trailing tails and that the gas is not unbound and lost to the surroundings unless the dwarf pair is residing near a massive galaxy. We conclude that a nearby, massive host galaxy is what ultimately prevents the gas from being re-accreted. Dwarf–dwarf interactions thus represent an important part of the baryon cycle of low-mass galaxies, enabling the 'parking' of gas at large distances to serve as a continual gas supply channel until accretion by a more massive host.

Dwarf galaxy problem

Dwarf spheroidal galaxy

Local Group

10.1093/mnras/stw757

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Citations (71)

Molecular and atomic gas along and across the main sequence of star-forming galaxies

Monthly Notices of the Royal Astronomical Society (2016)

A. Saintonge Barbara Catinella L. Cortese R. Genzel Riccardo Giovanelli

We use spectra from the ALFALFA, GASS and COLD GASS surveys to quantify variations in the mean atomic and molecular gas mass fractions throughout the SFR–M* plane and along the main sequence (MS) of star-forming galaxies. Although galaxies well below the MS tend to be undetected in the Arecibo and IRAM observations, reliable mean atomic and molecular gas fractions can be obtained through a spectral stacking technique. We find that the position of galaxies in the SFR–M* plane can be explained mostly by their global cold gas reservoirs as observed in the H i line, with in addition systematic variations in the molecular-to-atomic ratio and star formation efficiency. When looking at galaxies within ±0.4 dex of the MS, we find that as stellar mass increases, both atomic and molecular gas mass fractions decrease, stellar bulges become more prominent, and the mean stellar ages increase. Both star formation efficiency and molecular-to-atomic ratios vary little for massive MS galaxies, indicating that the flattening of the MS is due to the global decrease of the cold gas reservoirs of galaxies rather than to bottlenecks in the process of converting cold atomic gas to stars.

Flattening

10.1093/mnras/stw1715

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Citations (209)

Deriving a multivariate αCO conversion function using the [CII]/CO(1-0) ratio and its application to molecular gas scaling relations

Monthly Notices of the Royal Astronomical Society (2017)

Gioacchino Accurso A. Saintonge Barbara Catinella L. Cortese Romeel Davé

We present Herschel PACS observations of the [CII] 158 micron emission line in a sample of 24 intermediate mass (9

Stellar mass

10.1093/mnras/stx1556

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Citations (125)

Angular momentum regulates H igas content and H icentral hole size in the discs of spirals

Monthly Notices of the Royal Astronomical Society (2018)

C. Murugeshan V. A. Kilborn Danail Obreschkow Karl Glazebrook Katharina Lutz

The neutral atomic hydrogen (H i) content of spiral galaxies has been observed to vary with environment, with more H i-deficient spirals residing in high-density environments. This can be attributed to environmental effects such as ram pressure stripping and tidal interactions, which remove H i from the discs of galaxies. However, some spirals in low-density environments have also been observed to have relatively low H i mass fractions. The low densities of the intergalactic medium and lack of nearby galaxies in such environments make ram pressure stripping and tidal interactions unlikely candidates of gas removal. What then could be making these spirals H i deficient? Obreschkow et al. introduced a parameter-free model for the neutral atomic gas fraction (fatm), in a symmetric equilibrium disc as a function of the global atomic stability parameter (q), which depends on specific angular momentum. In order to examine if this model accounts for H i-deficient galaxies in low-density environments, we have used the |$M_{\rm H\; {\small I}}-$|MR scaling relation to select six H i-deficient spiral galaxies and observed them with the Australia Telescope Compact Array. By measuring their |$f_{\rm \small atm}$| and q values we find that the galaxies owe their observed H i deficiencies to low specific angular momenta. Additionally, we also find that the central H i hole sizes of our sample galaxies are related to their q values, following the prediction of Obreschkow et al. This result brings to light the importance of angular momentum in understanding the physics of the interstellar medium in the discs of galaxies and consequently their evolution.

Content (measure theory)

Ram pressure

Mass fraction

Stripping (fiber)

10.1093/mnras/sty3265

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Citations (29)

Erratum: The HIX galaxy survey II: HI kinematics of HI eXtreme galaxies

Monthly Notices of the Royal Astronomical Society (2018)

Katharina Lutz V. A. Kilborn B. Koribalski Barbara Catinella G. I. G. Józsa

10.1093/mnras/sty3423

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Citations (1)

The H ix galaxy survey – II. H i kinematics of H i eXtreme galaxies

Monthly Notices of the Royal Astronomical Society (2018)

Katharina Lutz V. A. Kilborn B. Koribalski Barbara Catinella G. I. G. Józsa

By analysing a sample of galaxies selected from the HI Parkes All Sky Survey (HIPASS) to contain more than 2.5 times their expected HI content based on their optical properties, we investigate what drives these HI eXtreme (HIX) galaxies to be so HI-rich. We model the HI kinematics with the Tilted Ring Fitting Code TiRiFiC and compare the observed HIX galaxies to a control sample of galaxies from HIPASS as well as simulated galaxies built with the semi-analytic model Dark Sage. We find that (1) HI discs in HIX galaxies are more likely to be warped and more likely to host HI arms and tails than in the control galaxies, (2) the average HI and average stellar column density of HIX galaxies is comparable to the control sample, (3) HIX galaxies have higher HI and baryonic specific angular momenta than control galaxies, (4) most HIX galaxies live in higher-spin haloes than most control galaxies. These results suggest that HIX galaxies are HI-rich because they can support more HI against gravitational instability due to their high specific angular momentum. The majority of the HIX galaxies inherits their high specific angular momentum from their halo. The HI content of HIX galaxies might be further increased by gas-rich minor mergers. This paper is based on data obtained with the Australia Telescope Compact Array (ATCA) through the large program C 2705.

Control sample

10.1093/mnras/sty387

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Citations (37)