scholarly journals H i asymmetries in LVHIS, VIVA, and HALOGAS galaxies

2020 ◽  
Vol 493 (4) ◽  
pp. 5089-5106 ◽  
Author(s):  
T N Reynolds ◽  
T Westmeier ◽  
L Staveley-Smith ◽  
G Chauhan ◽  
C D P Lagos
Keyword(s):  
Dynamic Range ◽  
Local Density ◽  
Neutral Hydrogen ◽  
Local Environment ◽  
Stellar Mass ◽  
Nearest Neighbour ◽  
L Band ◽  
Atomic Gas ◽  
Measures Of Asymmetry ◽  
The Impact

ABSTRACT We present an analysis of morphological, kinematic, and spectral asymmetries in observations of atomic neutral hydrogen (H i) gas from the Local Volume H i Survey (LVHIS), the VLA Imaging of Virgo in Atomic Gas (VIVA) survey, and the Hydrogen Accretion in Local Galaxies Survey. With the aim of investigating the impact of the local environment density and stellar mass on the measured H i asymmetries in future large H i surveys, we provide recommendations for the most meaningful measures of asymmetry for use in future analysis. After controlling for stellar mass, we find signs of statistically significant trends of increasing asymmetries with local density. The most significant trend we measure is for the normalized flipped spectrum residual (Aspec), with mean LVHIS and VIVA values of 0.204 ± 0.011 and 0.615 ± 0.068 at average weighted 10th nearest-neighbour galaxy number densities of log (ρ10/Mpc−3) = −1.64 and 0.88, respectively. Looking ahead to the Widefield ASKAP L-band Legacy All-sky Blind survey on the Australian Square Kilometre Array Pathfinder, we estimate that the number of detections will be sufficient to provide coverage over 5 orders of magnitude in both local density and stellar mass increasing the dynamic range and accuracy with which we can probe the effect of these properties on the asymmetry in the distribution of atomic gas in galaxies.

scholarly journals Recent star formation in the Hi dominated outer regions of early-type galaxies

2016 ◽  
Vol 11 (S321) ◽  
pp. 279-279
Author(s):  
Mustafa K. Yıldız ◽  
Paolo Serra ◽  
Reynier F. Peletier ◽  
Tom A. Oosterloo ◽  
Pierre-Alain Duc
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Radial Profile ◽  
Control Sample ◽  
Neutral Hydrogen ◽  
Stellar Mass ◽  
Early Type ◽  
Stellar Kinematics ◽  
The Impact

AbstractContextAccording to the ATLAS3D project, about 20 percent of all nearby early-type galaxies (D < 42 Mpc; MK < -21.5 mag; stellar mass Mstars ≳ 6 × 109 M⊙) outside clusters are surrounded by a disc or ring of low-column-density neutral hydrogen (Hi) gas with typical radii of tens of kpc, much larger than the stellar body.AimsOur aim is to understand the impact of these gas systems on the host galaxies, in particular, whether there is any recent star formation related to the Hi and effect of recent star formation on the host early-type galaxies.Methods and sampleWe analyse the distribution of star formation out to large radii by using resolved Hi images together with UV and optical images. We calculate the UV-UV and UV-optical colours in two apertures, 1-3 and 3-10 Reff. Using FUV emission as a proxy for star formation, we also estimate the integrated star formation rate in the outer regions. Our sample consists of 18 Hi-rich galaxies as well as 55 control galaxies where no Hi has been detected. We select the control sample galaxies to match the Hi-rich galaxies in stellar mass, environment, distance and stellar kinematics.ResultsIn half of the Hi-rich galaxies the radial UV profile changes slope at the position of the Hi radial profile peak. We find that the FUV-NUV and UV-optical colours in the first and second apertures of the Hi-rich galaxies are on average 0.5 and 0.8 mag bluer than the Hi-poor ones, respectively. We also find that the Hi-rich early-type galaxies have colour gradients that are almost 2 times stronger than the Hi-poor ones. we estimate the integrated star formation rate in the outer regions (R > 1 Reff) to be on average ~ 6.1×10−3 M⊙ yr−1 for the Hi-rich galaxies. We find that the gas depletion time in the outermost region (3-10 Reff) is ~ 80 Gyrs, which is similar to that estimated for the outskirts of spirals.ConclusionsStudying the stellar populations in early type galaxies with and without Hi, we find that galaxies with Hi generally show UV and UV-Optical colours in the outer parts that are bluer than those of early-type galaxies without Hi. This shows that the Hi is actively involved in recent star formation. The star formation rate in the outer regions is too low to build a stellar disc, and therefore change the morphology of the host even when integrated over several Gyrs. Star formation in outermost regions does not depend on the type of the galaxies.

scholarly journals Clues to the nature of dark matter from first galaxies

2019 ◽  
Vol 489 (1) ◽  
pp. 487-496 ◽  
Author(s):  
Boyan K Stoychev ◽  
Keri L Dixon ◽  
Andrea V Macciò ◽  
Marvin Blank ◽  
Aaron A Dutton
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Galaxy Formation ◽  
Cold Dark Matter ◽  
High Redshift ◽  
Formation Rate ◽  
Neutral Hydrogen ◽  
Mass Function ◽  
Stellar Mass ◽  
The Impact

ABSTRACT We use 38 high-resolution simulations of galaxy formation between redshift 10 and 5 to study the impact of a 3 keV warm dark matter (WDM) candidate on the high-redshift Universe. We focus our attention on the stellar mass function and the global star formation rate and consider the consequences for reionization, namely the neutral hydrogen fraction evolution and the electron scattering optical depth. We find that three different effects contribute to differentiate warm and cold dark matter (CDM) predictions: WDM suppresses the number of haloes with mass less than few 109 M⊙; at a fixed halo mass, WDM produces fewer stars than CDM, and finally at halo masses below 109 M⊙, WDM has a larger fraction of dark haloes than CDM post-reionization. These three effects combine to produce a lower stellar mass function in WDM for galaxies with stellar masses at and below 107 M⊙. For z > 7, the global star formation density is lower by a factor of two in the WDM scenario, and for a fixed escape fraction, the fraction of neutral hydrogen is higher by 0.3 at z ∼ 6. This latter quantity can be partially reconciled with CDM and observations only by increasing the escape fraction from 23 per cent to 34 per cent. Overall, our study shows that galaxy formation simulations at high redshift are a key tool to differentiate between dark matter candidates given a model for baryonic physics.

scholarly journals VIS3COS

2019 ◽  
Vol 630 ◽  
pp. A57 ◽  
Author(s):  
Ana Paulino-Afonso ◽  
David Sobral ◽  
Behnam Darvish ◽  
Bruno Ribeiro ◽  
Arjen van der Wel ◽  
...  
Keyword(s):  
Local Density ◽  
Elliptical Galaxies ◽  
Stellar Mass ◽  
High Density ◽  
Low Density ◽  
Star Forming ◽  
Structure And Morphology ◽  
Stellar Masses ◽  
The Impact ◽  
Non Parametric

We study the impact of local density and stellar mass on the structure and morphology of approximately 500 quiescent and star-forming galaxies from the VIMOS Spectroscopic Survey of a Superstructure in COSMOS (VIS3COS). We perform bulge-to-disc decomposition of the surface brightness profiles and find ∼41 ± 3% of > 1010 M⊙ galaxies to be best fitted with two components. We complement our analysis with non-parametric morphological measurements and qualitative visual classifications. We find that both galaxy structure and morphology depend on stellar mass and environment for our sample as a whole. We only find an impact of the environment on galaxy size for galaxies more massive than 1011 M⊙. We find higher Sérsic indices (n) and bulge-to-total ratios (B/T) in high-density regions when compared to low-density counterparts at similar stellar masses. We also find that galaxies with higher stellar mass have steeper light profiles (high n, B/T) compared to galaxies with lower stellar mass. Using visual classifications, we find a morphology–density relation at z ∼ 0.84 for galaxies more massive than 1010 M⊙, with elliptical galaxies being dominant at high-density regions and disc galaxies more common in low-density regions. However, when splitting the sample into colour–colour-selected star-forming and quiescent sub-populations, there are no statistically significant differences between low- and high-density regions. We find that quiescent galaxies are smaller, have higher Sérsic indices (for single profiles, around n ∼ 4), and higher bulge-to-total light ratios (for decomposed profiles, around B/T ∼ 0.5) when compared to star-forming counterparts (n ∼ 1 and B/T ∼ 0.3, for single and double profiles, respectively). We confirm these trends with non-parametric quantities, finding quiescent galaxies to be smoother (lower asymmetry, lower M20) and to have most of their light over smaller areas (higher concentration and Gini coefficient) than star-forming galaxies. Overall, we find a stronger dependence of structure and morphology on stellar mass than on local density and these relations are strongly correlated with the quenching fraction. The change in average structure or morphology corresponds to a change in the relative fractions of blue disc-like galaxies and red elliptical galaxies with stellar mass and environment. We hypothesise that the processes responsible for the quenching of star formation must also affect the galaxy morphology on similar timescales.

scholarly journals H i gas content of SDSS galaxies revealed by ALFALFA: implications for the mass–metallicity relation and the environmental dependence of H i in the local Universe

2020 ◽  
Vol 496 (1) ◽  
pp. 111-124 ◽  
Author(s):  
Ying Zu
Keyword(s):  
Star Formation ◽  
Formation Rate ◽  
Neutral Hydrogen ◽  
Mass Function ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Gas Content ◽  
Local Universe ◽  
The Impact ◽  
Environmental Dependence

ABSTRACT The neutral hydrogen (H i) gas is an important barometer of recent star formation and metal enrichment activities in galaxies. I develop a novel statistical method for predicting the H i-to-stellar mass ratio, $f_{\mathrm{H\,{\small I}}}$, of galaxies from their stellar mass and optical colour, and apply it to a volume-limited galaxy sample jointly observed by the Sloan Digital Sky Survey and the Arecibo Legacy Fast ALFA survey. I eliminate the impact of the Malmquist bias against H i-deficient systems on the $f_{\mathrm{H\,{\small I}}}$ predictor by properly accounting for the H i detection probability of each galaxy in the analysis. The best-fitting $f_{\mathrm{H\,{\small I}}}$ predictor, with an estimated scatter of 0.272 dex, provides excellent description to the observed H i mass function. After defining an H i excess parameter as the deviation of the observed $f_{\mathrm{H\,{\small I}}}$ from the expected value, I confirm that there exists a strong secondary dependence of the mass–metallicity relation on H i excess. By further examining the 2D metallicity distribution on the specific star formation rate (sSFR) versus H i excess plane, I show that the metallicity dependence on H i is likely more fundamental than that on sSFR. In addition, I find that the environmental dependence of H i in the local Universe can be effectively described by the cross-correlation coefficient between H i excess and the red galaxy overdensity ρcc = − 0.18. This weak anticorrelation also successfully explains the observed dependence of H i clustering on $f_{\mathrm{H\,{\small I}}}$. My method provides a useful framework for learning H i gas evolution from the synergy between future H i and optical galaxy surveys.

Dark matter content of ETGs and its relation to the local density of galaxies

2020 ◽  
Vol 15 (S359) ◽  
pp. 42-45
Author(s):  
A. Nigoche-Netro ◽  
G. Ramos-Larios ◽  
R. Díaz ◽  
E. de la Fuente ◽  
P. Lagos ◽  
...  
Keyword(s):  
Dark Matter ◽  
Local Density ◽  
Stellar Mass ◽  
Matter Content ◽  
Sloan Digital Sky Survey ◽  
Dynamical Mass ◽  
Sky Survey ◽  
The Impact ◽  
Mass Functions ◽  
Light Profiles

AbstractWe study the behaviour of the dynamical and stellar mass inside the effective radius as function of local density for early-type galaxies (ETGs). We use several samples of ETGs - ranging from 19000 to 98000 objects - from the ninth data release of the Sloan Digital Sky Survey. We consider Newtonian dynamics, different light profiles and different initial mass functions (IMF) to calculate the dynamical and stellar mass. We assume that any difference between these two masses is due to dark matter and/or a non-universal IMF. The main results are: (i) the amount of dark matter (DM) inside ETGs depends on the environment; (ii) ETGs in low-density environments span a wider DM range than ETGs in dense environments; (iii) the amount of DM inside ETGs in the most dense environments will be less than approximately 55-65 per cent of the dynamical mass; (iv) the accurate value of this upper limit depends on the impact of the IMF on the stellar mass estimation.

scholarly journals How robustly can we constrain the low-mass end of the z ∼ 6−7 stellar mass function? The limits of lensing models and stellar population assumptions in the Hubble Frontier Fields

2020 ◽  
Vol 501 (2) ◽  
pp. 1568-1590
Author(s):  
Lukas J Furtak ◽  
Hakim Atek ◽  
Matthew D Lehnert ◽  
Jacopo Chevallard ◽  
Stéphane Charlot
Keyword(s):  
Star Formation ◽  
Mass Function ◽  
Stellar Mass ◽  
Star Formation History ◽  
Space Telescope ◽  
Formation History ◽  
Low Mass ◽  
Stellar Masses ◽  
Dust Attenuation ◽  
The Impact

ABSTRACT We present new measurements of the very low mass end of the galaxy stellar mass function (GSMF) at z ∼ 6−7 computed from a rest-frame ultraviolet selected sample of dropout galaxies. These galaxies lie behind the six Hubble Frontier Field clusters and are all gravitationally magnified. Using deep Spitzer/IRAC and Hubble Space Telescope imaging, we derive stellar masses by fitting galaxy spectral energy distributions and explore the impact of different model assumptions and parameter degeneracies on the resulting GSMF. Our sample probes stellar masses down to $M_{\star }\gt 10^{6}\, \text{M}_{\odot}$ and we find the z ∼ 6−7 GSMF to be best parametrized by a modified Schechter function that allows for a turnover at very low masses. Using a Monte Carlo Markov chain analysis of the GSMF, including accurate treatment of lensing uncertainties, we obtain a relatively steep low-mass end slope $\alpha \simeq -1.96_{-0.08}^{+0.09}$ and a turnover at $\log (M_T/\text{M}_{\odot})\simeq 7.10_{-0.56}^{+0.17}$ with a curvature of $\beta \simeq 1.00_{-0.73}^{+0.87}$ for our minimum assumption model with constant star formation history (SFH) and low dust attenuation, AV ≤ 0.2. We find that the z ∼ 6−7 GSMF, in particular its very low mass end, is significantly affected by the assumed functional form of the star formation history and the degeneracy between stellar mass and dust attenuation. For example, the low-mass end slope ranges from $\alpha \simeq -1.82_{-0.07}^{+0.08}$ for an exponentially rising SFH to $\alpha \simeq -2.34_{-0.10}^{+0.11}$ when allowing AV of up to 3.25. Future observations at longer wavelengths and higher angular resolution with the James Webb Space Telescope are required to break these degeneracies and to robustly constrain the stellar mass of galaxies on the extreme low-mass end of the GSMF.

scholarly journals A Survey of Marine Coastal Litters around Zhoushan Island, China and Their Impacts

2021 ◽  
Vol 9 (2) ◽  
pp. 183
Author(s):  
Xuehua Ma ◽  
Yi Zhou ◽  
Luyi Yang ◽  
Jianfeng Tong
Keyword(s):  
Rapid Development ◽  
Univariate Analysis ◽  
Local Environment ◽  
Marine Litter ◽  
Social Ecological ◽  
The Social ◽  
Significant Difference ◽  
Valuable Method ◽  
Beach Litter ◽  
The Impact

Rapid development of the economy increased marine litter around Zhoushan Island. Social-ecological scenario studies can help to develop strategies to adapt to such change. To investigate the present situation of marine litter pollution, a stratified random sampling (StRS) method was applied to survey the distribution of marine coastal litters around Zhoushan Island. A univariate analysis of variance was conducted to access the amount of litter in different landforms that include mudflats, artificial and rocky beaches. In addition, two questionnaires were designed for local fishermen and tourists to provide social scenarios. The results showed that the distribution of litter in different landforms was significantly different, while the distribution of litter in different sampling points had no significant difference. The StRS survey showed to be a valuable method for giving a relative overview of beach litter around Zhoushan Island with less effort in a future survey. The questionnaire feedbacks helped to understand the source of marine litter and showed the impact on the local environment and economy. Based on the social-ecological scenarios, governance recommendations were provided in this paper.

scholarly journals “We Make Our Community”: Youth Forging Environmental Identities in Urban Landscapes

2021 ◽  
Vol 13 (14) ◽  
pp. 7736
Author(s):  
Erin Gallay ◽  
Alisa Pykett ◽  
Constance Flanagan
Keyword(s):  
High School Students ◽  
Urban Areas ◽  
Local Environment ◽  
Natural World ◽  
Urban Landscapes ◽  
Youth Of Color ◽  
School Students ◽  
Environmental Leadership ◽  
And Gender ◽  
The Impact

Insofar as race, class, and gender have profound effects on people’s environmental experiences, and consequently their activism, the environmental field needs more work on the environmental experiences and insights of groups whose voices have been missing, including youth of color who live in urban areas in the U.S. In this paper, we focus on African American and Latinx students engaged in environmental projects in their urban communities and the impact of such projects on promoting pro-environmental leadership, agency, and behavior. We draw from written reflections and focus group interviews of several hundred 4th–12th graders (majority middle- and high-school students) who participated in place-based civic science projects. Thematic analyses of student responses found that students engaged in work on local environmental issues cultivated an appreciation for the natural world and an understanding of human-nature interdependence and the ties between the local environment and their communities’ health. Through taking action with others in their communities, students viewed themselves as contributors to their communities and started to form environmental identities in ways that are not traditionally measured. Findings point to the need for forms of environmental education that are contextually grounded and centered on environmental justice in urban areas.

scholarly journals Erratum: Deconstructing the Galaxy stellar mass function with UKIDSS and CANDELS: the impact of colour, structure and environment

2016 ◽  
Vol 458 (4) ◽  
pp. 3478-3478 ◽  
Author(s):  
Alice Mortlock ◽  
Christopher. J. Conselice ◽  
William G. Hartley ◽  
Ken Duncan ◽  
Caterina Lani ◽  
...  
Keyword(s):  
Mass Function ◽  
Stellar Mass ◽  
The Galaxy ◽  
The Impact

POSSIBILITIES OF IMPLEMENTING THE SMART DEVELOPMENT CONCEPT IN RURAL AREAS FROM A BUSINESS PERSPECTIVE. THE EXAMPLE OF EASTERN POLAND

2021 ◽  
Vol XIII (1) ◽  
pp. 100-112
Author(s):  
Magdalena Anna Zwolińska-Ligaj
Keyword(s):  
Rural Areas ◽  
Institutional Environment ◽  
Descriptive Analysis ◽  
Smart Growth ◽  
Local Environment ◽  
Growth Potential ◽  
Opinion Poll ◽  
Local Sector ◽  
Endogenous Potential ◽  
The Impact

The aim of this paper was the evaluation of the impact of selected background conditions for implementing the smart village concept in the opinion of entrepreneurs. The assessment was based on an opinion poll on a sample of 240 entrepreneurs from three regions of Eastern Poland, using a questionnaire. The results were presented using descriptive analysis, including a comparative analysis of areas with low and high levels of smart growth potential. The presented results show that rural areas in the abovementioned regions, in general, create disadvantageous conditions for enhancing innovativeness through business activity, and the surveyed agents are characterised by a low level of innovativeness. In the opinion of the surveyed entrepreneurs, on the impact of selected factors on enterprise innovativeness, the potential impact of the local environment is above average. The findings point to a need to develop the endogenous potential of rural areas from peripheral regions by increasing access to modern ITC infrastructure and the role of the institutional environment in the process of knowledge transfer to the local sector of companies, the development of local connections in the business sector and within the scope of cooperation of local authorities with entrepreneurs.

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