154 research outputs found
Probing galaxy evolution through HI 21-cm emission and absorption: current status and prospects with the Square Kilometre Array
One of the major science goals of the Square Kilometre Array (SKA) is to
understand the role played by atomic hydrogen (HI) gas in the evolution of
galaxies throughout cosmic time. The hyperfine transition line of the hydrogen
atom at 21-cm is one of the best tools to detect and study the properties of HI
gas associated with galaxies. In this article, we review our current
understanding of HI gas and its relationship with galaxies through observations
of the 21-cm line both in emission and absorption. In addition, we provide an
overview of the HI science that will be possible with SKA and its pre-cursors
and pathfinders, i.e. HI 21-cm emission and absorption studies of galaxies from
nearby to high redshifts that will trace various processes governing galaxy
evolution.Comment: 31 pages, 7 figures, accepted on 27 May 2022 for publication in the
Journal of Astrophysics and Astronomy (to appear in the special issue on
"Indian participation in the SKA"), figure 4 has been update
MIGHTEE-H I: the MH I – M* relation over the last billion years
We study the MHI−M⋆ relation over the last billion years using the MIGHTEE-H i sample. We first model the upper envelope of the MHI−M⋆ relation with a Bayesian technique applied to a total number of 249 H i-selected galaxies, without binning the datasets, while taking account of the intrinsic scatter. We fit the envelope with both linear and non-linear models, and find that the non-linear model is preferred over the linear one with a measured transition stellar mass of log10 (M⋆M⊙) = 9.15±0.87, beyond which the slope flattens. This finding supports the view that the lack of H i gas is ultimately responsible for the decreasing star formation rate observed in the massive main-sequence galaxies. For spirals alone, which are biased towards the massive galaxies in our sample, the slope beyond the transition mass is shallower than for the full sample, indicative of distinct gas processes ongoing for the spirals/high-mass galaxies from other types with lower stellar masses. We then create mock catalogues for the MIGHTEE-H i detections and non-detections with two main galaxy populations of late- and early-type galaxies to measure the underlying MHI−M⋆ relation. We find that the turnover in this relation persists whether considering the two galaxy populations as a whole or separately. We note that an underlying linear relation could mimic this turnover in the observed scaling relation, but a model with a turnover is strongly preferred. Measurements on the logarithmic average of H i masses against the stellar mass are provided as a benchmark for future studies
MIGHTEE-HI: the HI Size-Mass relation over the last billion years
We present the observed HI size-mass relation of galaxies from the
MIGHTEE Survey Early Science data. The high sensitivity of MeerKAT allows us to
detect galaxies spanning more than 4 orders of magnitude in HI mass, ranging
from dwarf galaxies to massive spirals, and including all morphological types.
This is the first time the relation has been explored on a blind homogeneous
data set which extends over a previously unexplored redshift range of , i.e. a period of around one billion years in cosmic time. The sample
follows the same tight logarithmic relation derived from previous work, between
the diameter () and the mass () of HI discs. We measure
a slope of , an intercept of , and an
observed scatter of dex. For the first time, we quantify the intrinsic
scatter of dex (), which provides a constraint
for cosmological simulations of galaxy formation and evolution. We derive the
relation as a function of galaxy type and find that their intrinsic scatters
and slopes are consistent within the errors. We also calculate the relation for two redshift bins and do not find any evidence for
evolution with redshift. These results suggest that over a period of one
billion years in lookback time, galaxy discs have not undergone significant
evolution in their gas distribution and mean surface mass density, indicating a
lack of dependence on both morphological type and redshift.Comment: 10 pages, 5 figures, accepted for publication in MNRA
MIGHTEE-HI: The first MeerKAT HI mass function from an untargeted interferometric survey
We present the first measurement of the HI mass function (HIMF) using data
from MeerKAT, based on 276 direct detections from the MIGHTEE Survey Early
Science data covering a period of approximately a billion years (). This is the first HIMF measured using interferometric data over
non-group or cluster field, i.e. a deep blank field. We constrain the
parameters of the Schechter function which describes the HIMF with two
different methods: and Modified Maximum Likelihood (MML).
We find a low-mass slope , `knee' mass
and normalisation
(
kms Mpc) for and
, `knee' mass and normalisation for MML. When using we
find both the low-mass slope and `knee' mass to be consistent within
with previous studies based on single-dish surveys. The cosmological mass
density of HI is found to be slightly larger than previously reported:
from and from MML but consistent within the uncertainties. We find
no evidence for evolution of the HIMF over the last billion years.Comment: 13 pages, 9 figures, accepted for publication in MNRA
MIGHTEE-HI: HI galaxy properties in the large scale structure environment at z ∼ 0.37 from a stacking experiment
We present the first measurement of HI mass of star-forming galaxies in different large scale structure environments from a blind survey at z ∼ 0.37. In particular, we carry out a spectral line stacking analysis considering 2875 spectra of colour-selected star-forming galaxies undetected in HI at 0.23 < z < 0.49 in the COSMOS field, extracted from the MIGHTEE-HI Early Science datacubes, acquired with the MeerKAT radio telescope. We stack galaxies belonging to different subsamples depending on three different definitions of large scale structure environment: local galaxy overdensity, position inside the host dark matter halo (central, satellite, or isolated), and cosmic web type (field, filament, or knot). We first stack the full star-forming galaxy sample and find a robust HI detection yielding an average galaxy HI mass of MHI = (8.12 ± 0.75) × 109 M⊙ at ∼11.8σ. Next, we investigate the different subsamples finding a negligible difference in MHI as a function of the galaxy overdensity. We report an HI excess compared to the full sample in satellite galaxies (MHI = (11.31 ± 1.22) × 109, at ∼10.2σ) and in filaments (MHI = (11.62 ± 0.90) × 109. Conversely, we report non-detections for the central and knot galaxies subsamples, which appear to be HI-deficient. We find the same qualitative results also when stacking in units of HI fraction (fHI). We conclude that the HI amount in star-forming galaxies at the studied redshifts correlates with the large scale structure environment
MIGHTEE-HI: HI galaxy properties in the large scale structure environment at z~0.37 from a stacking experiment
We present the first measurement of HI mass of star-forming galaxies in
different large scale structure environments from a blind survey at . In particular, we carry out a spectral line stacking analysis
considering spectra of colour-selected star-forming galaxies undetected
in HI at in the COSMOS field, extracted from the MIGHTEE-HI
Early Science datacubes, acquired with the MeerKAT radio telescope. We stack
galaxies belonging to different subsamples depending on three different
definitions of large scale structure environment: local galaxy overdensity,
position inside the host dark matter halo (central, satellite, or isolated),
and cosmic web type (field, filament, or knot). We first stack the full
star-forming galaxy sample and find a robust HI detection yielding an average
galaxy HI mass of at
. Next, we investigate the different subsamples finding a
negligible difference in as a function of the galaxy overdensity.
We report an HI excess compared to the full sample in satellite galaxies
(, at ) and in
filaments (. Conversely, we report
non-detections for the central and knot galaxies subsamples, which appear to be
HI-deficient. We find the same qualitative results also when stacking in units
of HI fraction (). We conclude that the HI amount in star-forming
galaxies at the studied redshifts correlates with the large scale structure
environment.Comment: Accepted for publication in MNRAS. 15 figures, 3 table
Agile Manifesto and Practices Selection for Tailoring Software Development: A Systematic Literature Review
peer reviewedAgile methods have been largely used for many years to provide developers with a flexible software development process leading to software quality improvement. To get the best results and eliminate unnecessary efforts, the development team should select the most appropriate methods and techniques. The fundamental core of an agile method has to be well-understood before deciding which parts of the method need to be adopted. We believe that the quickest way to do so is to understand the prescripts of the Agile Manifesto. Many researches have proposed different tailoring approaches based on the relation and straight-forward interpretation between each agile practice and agile values or principles. We however have observed that agile practitioners do not dedicate the necessary attention to the Agile Manifesto before adopting agile methods or practices and directly use them. It is because the importance of Agile Manifesto in tailoring context is not obvious enough to the community. This study aims at doing a systematic literature review on the existing case studies, to verify the relation between the Agile Manifesto and agile practice selection
Degradation behaviors and mechanisms of MoS2 crystals relevant to bioabsorbable electronics
Monolayer molybdenum disulfide (MoS2) exhibits unique semiconducting and bioresorption properties, giving this material enormous potential for electronic/biomedical applications, such as bioabsorbable electronics. In this regard, understanding the degradation performance of monolayer MoS2 in biofluids allows modulation of the properties and lifetime of related bioabsorbable devices and systems. Herein, the degradation behaviors and mechanisms of monolayer MoS2 crystals with different misorientation angles are explored. High-angle grain boundaries (HAGBs) biodegrade faster than low-angle grain boundaries (LAGBs), exhibiting degraded edges with wedge and zigzag shapes, respectively. Triangular pits that formed in the degraded grains have orientations opposite to those of the parent crystals, and these pits grow into larger pits laterally. These behaviors indicate that the degradation is induced and propagated based on intrinsic defects, such as grain boundaries and point defects, because of their high chemical reactivity due to lattice breakage and the formation of dangling bonds. High densities of dislocations and point defects lead to high chemical reactivity and faster degradation. The structural cause of MoS2 degradation is studied, and a feasible approach to study changes in the properties and lifetime of MoS2 by controlling the defect type and density is presented. The results can thus be used to promote the widespread use of two-dimensional materials in bioabsorption applications
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