69 research outputs found
HI scaling relations of galaxies in the environment of HI-rich and control galaxies observed by the Bluedisk project
Our work is based on the "Bluedisk" project, a program to map the neutral gas
in a sample of 25 HI-rich spirals and a similar number of control galaxies with
the Westerbork Synthesis Radio Telescope (WSRT). In this paper we focus on the
HI properties of the galaxies in the environment of our targeted galaxies. In
total, we extract 65 galaxies from the WSRT cubes with stellar masses between
and . Most of these galaxies are located on
the same HI mass-size relation and "HI-plane" as normal spiral galaxies. We
find that companions around HI-rich galaxies tend to be HI-rich as well and to
have larger R90,HI/R50,HI. This suggests a scenario of "HI conformity", similar
to the colour conformity found by Weinmann et al. (2006): galaxies tend to
adopt the HI properties of their neighbours. We visually inspect the outliers
from the HI mass-size relation and galaxies which are offset from the HI plane
and find that they show morphological and kinematical signatures of recent
interactions with their environment. We speculate that these outliers have been
disturbed by tidal or ram-pressure stripping processes, or in a few cases, by
accretion events.Comment: 16 pages, 12 figures; accepted for publication in MNRA
Bar-induced central star formation as revealed by integral field spectroscopy from CALIFA
We investigate the recent star formation history (SFH) in the inner region of
57 nearly face-on spiral galaxies selected from the Calar Alto Legacy Integral
Field Area (CALIFA) survey. For each galaxy we use the integral field
spectroscopy from CALIFA to obtain two-dimensional maps and radial profiles of
three parameters that are sensitive indicators of the recent SFH: the 4000\AA\
break (D(4000)), and the equivalent width of H absorption
(EW(H)) and H emission (EW(H)). We have also
performed photometric decomposition of bulge/bar/disk components based on SDSS
optical image. We identify a class of 17 "turnover" galaxies whose central
region present significant drop in D(4000), and most of them
correspondingly show a central upturn in EW(H) and EW(H).
This indicates that the central region of the turnover galaxies has experienced
star formation in the past 1-2 Gyr, which makes the bulge younger and more
star-forming than surrounding regions. We find almost all (15/17) the turnover
galaxies are barred, while only half of the barred galaxies in our sample
(15/32) are classified as a turnover galaxy. This finding provides strong
evidence in support of the theoretical expectation that the bar may drive gas
from the disc inward to trigger star formation in galaxy center, an important
channel for the growth/rejuvenation of pseudobulges in disc galaxies.Comment: 19 pages, 10 figures, ApJ accepte
The Formation of Star-forming Disks in the TNG50 Simulation
We investigate the disk formation process in the TNG50 simulation, examining
the profiles of SFR surface density (), gas inflow and
outflow, and the evolution of the angular momentum of inflowing gas particles.
The TNG50 galaxies tend to have larger star-forming disks, and also show larger
deviations from exponential profiles in when compared to
real galaxies in the MaNGA (Mapping Nearby Galaxies at APO) survey. The stellar
surface density of TNG50 galaxies show good exponential profiles, which is
found to be the result of strong radial migration of stars over time. However,
this strong radial migration of stars in the simulation produces flatter age
profiles in TNG50 disks compared to observed galaxies. The star formation in
the simulated galaxies is sustained by a net gas inflow and this gas inflow is
the primary driver for the cosmic evolution of star formation, as expected from
simple gas-regulator models of galaxies. There is no evidence for any
significant loss of angular momentum for the gas particles after they are
accreted on to the galaxy, which may account for the large disk sizes in the
TNG50 simulation. Adding viscous processes to the disks, such as the magnetic
stresses from magneto-rotational instability proposed by Wang & Lilly 2022,
will likely reduce the sizes of the simulated disks and the tension with the
sizes of real galaxies, and may produce more realistic exponential profiles.Comment: 24 pages, 14 figures, accepted in Ap
The peculiar filamentary HI structure of NGC 6145
In this paper, we report the peculiar HI morphology of the cluster spiral
galaxy NGC 6145, which has a 150 kpc HI filament on one side that is nearly
parallel to its major axis. This filament is made up of several HI clouds and
the diffuse HI gas between them, with no optical counterparts. We compare its
HI distribution with other one-sided HI distributions in the literature, and
find that the overall HI distribution is very different from the typical tidal
and ram-pressure stripped HI shape, and its morphology is inconsistent with
being a pure accretion event. Only about 30% of the total HI gas is anchored on
the stellar disk, while most of HI gas forms the filament in the west. At a
projected distance of 122 kpc, we find a massive elliptical companion (NGC
6146) with extended radio emission, whose axis points to an HI gap in NGC 6145.
The velocity of the HI filament shows an overall light-of- sight motion of 80
to 180 km/s with respect to NGC 6145. Using the long-slit spectra of NGC 6145
along its major stellar axis, we find that some outer regions show enhanced
star formation, while in contrast, almost no star formation activities are
found in its center (less than 2 kpc). Pure accretion, tidal or ram-pressure
stripping is not likely to produce the observed HI filament. An alternative
explanation is the jet-stripping from NGC 6146, although direct evidence for a
jet-cold gas interaction has not been found.Comment: 12 pages, 6 figures; Accepted for publication in A
Spectroscopic Observation and Analysis of HII regions in M33 with MMT: Temperatures and Oxygen Abundances
The spectra of 413 star-forming (or HII) regions in M33 (NGC 598) were
observed by using the multifiber spectrograph of Hectospec at the 6.5-m
Multiple Mirror Telescope (MMT). By using this homogeneous spectra sample, we
measured the intensities of emission lines and some physical parameters, such
as electron temperatures, electron densities, and metallicities. Oxygen
abundances were derived via the direct method (when available) and two
empirical strong-line methods, namely, O3N2 and N2. In the high-metallicity
end, oxygen abundances derived from O3N2 calibration were higher than those
derived from N2 index, indicating an inconsistency between O3N2 and N2
calibrations. We presented a detailed analysis of the spatial distribution of
gas-phase oxygen abundances in M33 and confirmed the existence of the
axisymmetric global metallicity distribution widely assumed in literature.
Local variations were also observed and subsequently associated with spiral
structures to provide evidence of radial migration driven by arms. Our O/H
gradient fitted out to 1.1 resulted in slopes of ,
, and dex utilizing abundances from
O3N2, N2 diagnostics, and direct method, respectively.Comment: Accepted for publication in Ap
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