783 research outputs found
The HI Chronicles of LITTLE THINGS BCDs: Evidence for External Perturbations in the Morphology and Kinematics of Haro 29 and Haro 36
We analyze high angular and velocity resolution HI-line data of two LITTLE
THINGS (1) blue compact dwarfs (BCDs): Haro 29 and Haro 36. Both of these BCDs
are disturbed morphologically and kinematically. Haro 29's HI data reveal a
kinematic major axis that is offset from the optical major axis, and a
disturbed outer HI component, indicating that Haro 29 may have had a past
interaction. Position-velocity diagrams of Haro 36 indicate that it has two
kinematically separate components at its center and a likely tidal tail in
front of the galaxy. We find that Haro 36 most likely had an interaction in the
past, is currently interacting with an unknown companion, or is a merger
remnant. (1) "Local Irregulars That Trace Luminosity Extremes The HI Nearby
Galaxy Survey" http://www2.lowell.edu/users/dah/littlethings/index.htmlComment: To be published in The Astronomical Journa
The HI Chronicles of LITTLE THINGS BCDs II: The Origin of IC 10's HI Structure
In this paper we analyze Very Large Array (VLA) telescope and Green Bank
Telescope (GBT) atomic hydrogen (HI) data for the LITTLE THINGS(1) blue compact
dwarf galaxy IC 10. The VLA data allow us to study the detailed HI kinematics
and morphology of IC 10 at high resolution while the GBT data allow us to
search the surrounding area at high sensitivity for tenuous HI. IC 10's HI
appears highly disturbed in both the VLA and GBT HI maps with a kinematically
distinct northern HI extension, a kinematically distinct southern plume, and
several spurs in the VLA data that do not follow the general kinematics of the
main disk. We discuss three possible origins of its HI structure and kinematics
in detail: a current interaction with a nearby companion, an advanced merger,
and accretion of intergalactic medium. We find that IC 10 is most likely an
advanced merger or a galaxy undergoing accretion.
1:Local Irregulars That Trace Luminosity Extremes, The HI Nearby Galaxy
Survey; https://science.nrao.edu/science/surveys/littlethingsComment: 36 pages, 17 figures, accepted for publication in The Astronomical
Journa
DDO 88: A Galaxy-Sized Hole in the Interstellar Medium
We present an HI and optical study of the gas-rich dwarf irregular galaxy DDO
88. Although DDO 88's global optical and HI parameters are normal for its
morphological type, it hosts a large (3 kpc diameter) and unusually complete
ring of enhanced HI emission. The gas ring is located at approximately
one-third of the total HI radius and one-half the optically-defined Holmberg
radius, and contains 30% of the total HI of the galaxy. The ring surrounds a
central depression in the HI distribution, so it may be a shell formed by a
starburst episode. However, the UBV colors in the HI hole are not bluer than
the rest of the galaxy as would be expected if an unusual star-forming event
had taken place there recently, but there is an old (~1-3 Gyr), red cluster
near the center of the hole that is massive enough to have produced the hole in
the HI. An age estimate for the ring, however, is uncertain because it is not
observed to be expanding. An expansion model produces a lower estimate of 0.5
Gyr, but the presence of faint star formation regions associated with the ring
indicate a much younger age. We also estimate that the ring could have
dispersed by now if it is older than 0.5 Gyr. This implies that the ring is
younger than 0.5 Gyr. A younger age would indicate that the red cluster did not
produce the hole and ring. If this ring and the depression in the gas which it
surrounds were not formed by stellar winds and supernovae, this would indicate
that some other, currently unidentified, mechanism is operating.Comment: 44 pages; 16 figures. To appear in AJ, January 2005. Available from
ftp.lowell.edu, cd pub/dah/papers/d88 and http://www.fiu.edu/~simpsonc/d8
NGC 5291: Implications for the Formation of Dwarf Irregular Galaxies
The possible formation and evolution of dwarf irregular galaxies from material derived from perturbed evolved galaxies is addressed via an HI study of a likely example, the peculiar system NGC 5291. This system, located in the western outskirts of the cluster Abell 3574, contains the lenticular galaxy NGC 5291 which is in close proximity to a disturbed companion and is flanked by an extensive complex of numerous knots extending roughly 4\u27 north and 4\u27 south of the galaxy. In an initial optical and radio study, Longmore et al. (1979, MNRAS, 188, 285) showed that these knots have the spectra of vigorous star-forming regions, and suggested that some may in fact be young dwarf irregular galaxies. High resolution 21-cm line observations taken with the VLA are presented here and reveal that the H I distribution associated with this system encompasses not only the entire N-S complex of optical knots, but also forms an incomplete ring or tail that extends approximately 3\u27 to the west. The HI associated with NGC 5291 itself shows a high velocity range; the Seashell is not detected. The formation mechanism for this unusual system is unclear and two models-a large, low-luminosity ram-swept disk, and a ram-swept interaction-are discussed. The HI in the system contains numerous concentrations, mostly along the N-S arc of the star-forming complexes, which generally coincide with one or more optical knots; the larger HI features contain several X 109 M0 of gas. Each of the knots is compared to a set of criteria designed to determine if these objects are bound against their own internal kinetic energy and are tidally stable relative to the host galaxy. An analysis of the properties of the H I concentrations surrounding the optical star-forming complexes indicates that at least the largest of these is a bound system; it also possesses a stellar component. It is suggested that this object is a genuinely young dwarf irregular galaxy that has evolved from the material associated with the system and that this entire complex contains several proto- or young dwarf irregular galaxies in various stages of development. We are therefore witnessing the early evolution of a number of genuinely young galaxies. Given the evident importance of the NGC 5291 system as a \u27\u27nursery\u27\u27 for young galaxies, careful modeling is required if we are to understand this remarkable galaxy
VII Zw 403: H I structure in a blue compact dwarf galaxy
‘In these times, during the rise in the popularity of institutional repositories, the Society does not forbid authors from depositing their work in such repositories. However, the AAS regards the deposit of scholarly work in such repositories to be a decision of the individual scholar, as long as the individual's actions respect the diligence of the journals and their reviewers.’ Original article can be found at : http://iopscience.iop.org/ Copyright American Astronomical SocietyWe present optical (UBVJ), ultraviolet (FUV, NUV), and high-resolution atomic hydrogen (H I) observations of the nearby blue compact dwarf (BCD), VII Zw 403. We find that VII Zw 403 has a relatively high H I mass-to-light ratio for a BCD. The rotation velocity is nominally 10-15 km s(-1), but rises to similar to 20 km s(-1) after correction for the similar to 8-10 km s(-1) random motions present in the gas. The velocity field is complex, including a variation in the position angle of the major axis going from the northeast to the southwest parts of the galaxy. Our high-resolution Hi maps reveal structure in the central gas, including a large, low-density Hi depression or hole between the southern and northern halves of the galaxy, coincident with an unresolved X-ray source. Although interactions have been proposed as the triggering mechanism for the vigorous star formation occurring in BCDs, VII Zw 403 does not seem to have been tidally triggered by an external interaction, as we have found no nearby possible perturbers. It also does not appear to fall in the set of galaxies that exhibit a strong central mass density concentration, as its optical scale length is large in comparison to similar systems. However, there are some features that are compatible with an accretion event: optical/Hi axis misalignment, a change in position angle of the kinematic axis, and a complex velocity field.Peer reviewe
A Search for correlations between turbulence and star formation in LITTLE THINGS dwarf irregular galaxies
Turbulence has the potential for creating gas density enhancements that
initiate cloud and star formation (SF), and it can be generated locally by SF.
To study the connection between turbulence and SF, we looked for relationships
between SF traced by FUV images, and gas turbulence traced by kinetic energy
density (KED) and velocity dispersion () in the LITTLE THINGS sample
of nearby dIrr galaxies. We performed 2D cross-correlations between FUV and KED
images, measured cross-correlations in annuli to produce correlation
coefficients as a function of radius, and determined the cumulative
distribution function of the cross correlation value. We also plotted on a
pixel-by-pixel basis the locally excess KED, , and HI mass surface
density, , as determined from the respective values with the
radial profiles subtracted, versus the excess SF rate density , for all regions with positive excess . We found that
and KED are poorly correlated. The excess KED associated
with SF implies a % efficiency for supernova energy to pump local HI
turbulence on the scale of resolution here, which is a factor of too
small for all of the turbulence on a galactic scale. The excess in
SF regions is also small, only km s. The local excess in
corresponding to an excess in is
consistent with an HI consumption time of Gyr in the inner parts of
the galaxies. The similarity between this timescale and the consumption time
for CO implies that CO-dark molecular gas has comparable mass to HI in the
inner disks.Comment: In press in the Astronomical Journa
A Search for Correlations between Turbulence and Star Formation in LITTLE THINGS Dwarf Irregular Galaxies
Turbulence has the potential for creating gas density enhancements that initiate cloud and star formation (SF), and it can be generated locally by SF. To study the connection between turbulence and SF, we looked for relationships between SF traced by FUV images, and gas turbulence traced by kinetic energy density (KED) and velocity dispersion (v disp) in the LITTLE THINGS sample of nearby dIrr galaxies. We performed 2D cross-correlations between FUV and KED images, measured cross-correlations in annuli to produce correlation coefficients as a function of radius, and determined the cumulative distribution function of the cross-correlation value. We also plotted on a pixel-by-pixel basis the locally excess KED, v disp, and H i mass surface density, ΣHI, as determined from the respective values with the radial profiles subtracted, versus the excess SF rate density ΣSFR, for all regions with positive excess ΣSFR. We found that ΣSFR and KED are poorly correlated. The excess KED associated with SF implies a ∼0.5% efficiency for supernova energy to pump local H i turbulence on the scale of the resolution here, which is a factor of ∼2 too small for all of the turbulence on a galactic scale. The excess v disp in SF regions is also small, only ∼0.37 km s-1. The local excess in ΣHI corresponding to an excess in ΣSFR is consistent with a H i consumption time of ∼1.6 Gyr in the inner parts of the galaxies. The similarity between this timescale and the consumption time for CO implies that CO-dark molecular gas has comparable mass to H i in the inner disks
Procedures for A Comparison of Electronic and Paper Versions of the Montreal Cognitive Assessment
Objective: To investigate older adults’ performance on the paper and electronic Montreal Cognitive Assessment (MoCA). We hypothesized the paper MoCA scores would be significantly higher than electronic MoCA (eMoCA) scores.
Design: Repeated measures and correlational design.
Setting: General community and university clinic.
Participants: A convenience sample of 40 adults over 65 years of age living in the community.
Interventions: Participants completed the eMoCA and paper MoCA in a randomized order during a single session. Participants reported their touchscreen experience and comfort, and indicated their administration modality preferences.
Main Outcome Measures: The primary outcome measures were Paper MoCA and eMoCA total and subscale scores. Secondary outcome measures included participants reported touchscreen experience and comfort, as well as post administration preferences.
Results: A moderate statistically significant correlation was found between performance on the eMoCA and the paper MoCA across all participants. Analysis comparing first administration modality only (eMoCA versus paper MoCA) found that there was not a statistically significant difference in total scores, however there was a statistically significant difference for the visuospatial/executive subscale, which required the test taker to physically interact with either the paper or the tablet. Across all subjects, there was a statistically significant correlation between experience with touchscreen devices and performance on the eMoCA, but not between modality preference and performance.
Conclusion: Modality of administration can impact performance on assessments of cognition. Clinicians should consider the amount of experience with touchscreens prior to deciding which modality to use with a client
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