scholarly journals Spectroscopic Analysis of Star-forming Regions in the Spiral Galaxy NGC 628

2022 ◽  
Vol 6 (1) ◽  
pp. 7
Author(s):  
Atharva Gorantiwar ◽  
Evan Skillman ◽  
Noah Rogers
Keyword(s):  
Chemical Composition ◽  
Chemical Analysis ◽  
Spiral Galaxy ◽  
Spectroscopic Analysis ◽  
Spiral Galaxies ◽  
Iron Line ◽  
Star Forming ◽  
Star Forming Regions ◽  
Methods Of Analysis ◽  
Contamination Problem

Abstract NGC 628 is one of many spiral galaxies that has been observed and analyzed to determine the chemical composition. Since there have been improvements in the methods of analysis recently, this paper finds new values for the electron temperatures within this galaxy. Additionally, it brings up a previously unnoticed iron line contamination problem that has affected the [O iii] temperatures and fluxes. Temperature results are compared against, the most recent chemical analysis of the same galaxy.

scholarly journals Spiral Galaxy in 3D as Seen with SpIOMM

2014 ◽  
Vol 10 (S309) ◽  
pp. 340-340
Author(s):  
Laurie Rousseau-Nepton ◽  
Carmelle Robert ◽  
Laurent Drissen
Keyword(s):  
Fourier Transform ◽  
Spatial Resolution ◽  
Spiral Galaxy ◽  
Spiral Galaxies ◽  
High Spatial Resolution ◽  
Large Database ◽  
Star Forming ◽  
Star Forming Regions ◽  
Warm Ionized Medium

AbstractUsing the imaging Fourier transform spectrograph (FTS) SpIOMM we study 7 nearby spiral galaxies. The large database of spectra obtained around Hα and Hβ is ideal to study the star forming regions and warm ionized medium (WIM) with a high spatial resolution (∼ 50-150 pc).

Simulating star-forming regions in spiral galaxies with AMUSE

2019 ◽  
Vol 14 (S351) ◽  
pp. 216-219
Author(s):  
Steven Rieder ◽  
Clare Dobbs ◽  
Thomas Bending
Keyword(s):  
Gas Dynamics ◽  
Molecular Clouds ◽  
Spiral Galaxies ◽  
Initial Conditions ◽  
Cluster Formation ◽  
Star Cluster ◽  
Star Forming ◽  
Star Forming Regions ◽  
Formation And Evolution ◽  
Spiral Arm

AbstractWe present a model for hydrodynamic + N-body simulations of star cluster formation and evolution using AMUSE. Our model includes gas dynamics, star formation in regions of dense gas, stellar evolution and a galactic tidal spiral potential, thus incorporating most of the processes that play a role in the evolution of star clusters.We test our model on initial conditions of two colliding molecular clouds as well as a section of a spiral arm from a previous galaxy simulation.

scholarly journals An X-Ray View of Interacting Binaries Outside The Galaxy

2004 ◽  
Vol 194 ◽  
pp. 3-6
Author(s):  
Andrea H. Prestwich
Keyword(s):  
Supernova Remnants ◽  
Luminosity Function ◽  
Local Group ◽  
Spiral Galaxies ◽  
High Mass ◽  
X Ray ◽  
Star Forming ◽  
Star Forming Regions ◽  
Low Mass ◽  
X Ray Binaries

AbstractChandra and XMM-Newton are revolutionizing our understanding of compact binaries in external galaxies, allowing us to study sources in detail in Local Group Galaxies and study populations in more distant systems. In M31 the X-ray luminosity function depends on the local stellar population in the sense that areas with active star formation have more high luminosity sources, and a higher overall source density (Kong. Di Stefano. Garcia, & Greiner 2003). This result is also true in galaxies outside the Local Group; starburst galaxies have flatter X-ray luminosity functions than do spiral galaxies which are in turn flatter than elliptical galaxies. These observational results suggest that the high end of the luminosity function in star forming regions is dominated by short-lived high mass X-ray binaries.In Chandra Cycle 2 we started a Large Project to survey a sample of 11 nearby (< 10Mpc) face-on spiral galaxies. We find that sources can be approximately classified on the basis of their X-ray color into low mass X-ray binaries, high mass X-ray binaries and supersoft sources. There is an especially interesting class of source that has X-ray colors softer (“redder”) than a typical low mass X-ray binary source, but not so extreme as supersoft sources. Most of these are probably X-ray bright supernova remnants, but some may be a new type of black hole accretor. Finally, when we construct a luminosity function of sources selecting only sources with low mass X-ray binary colors (removing soft sources) we find that there is a dip or break probably associated with the Eddington luminosity for a neutron star.

scholarly journals Stellar Populations in the Nuclei of Spiral Galaxies

1983 ◽  
Vol 6 ◽  
pp. 147-156 ◽  
Author(s):  
R. W. O’Connell
Keyword(s):  
Spiral Galaxies ◽  
Stellar Populations ◽  
Potential Well ◽  
Interstellar Gas ◽  
Central Potential ◽  
Star Forming ◽  
Star Forming Regions

Spiral galaxies are a composite of two dynamical population types: the spheroidal and disk populations. These can be studied in isolation in E and Irr galaxies, respectively. It is natural to expect that the combination in a spiral of a dense spheroidal population, having a deep central potential well, with a repository of interstellar gas and dust in the disk gives rise to special conditions not usually found in E or Irr galaxies. And in fact, we find spectacular concentrations of star forming regions in some spiral nuclei.In this review, I will limit most of the discussion to later spiral types which are classified as “intermediate” in the Yerkes system (Morgan and Osterbrock 1969). Types earlier than Sbc usually have “k-nuclei,” where the spheroidal population dominates; excellent reviews are available for these types (van den Bergh 1975, Faber 1977).

scholarly journals The Nuclear Ring in the Barred Spiral Galaxy IC 4933

2010 ◽  
Vol 27 (1) ◽  
pp. 56-63 ◽  
Author(s):  
Stuart D. Ryder ◽  
Samuel M. Illingworth ◽  
Robert G. Sharp ◽  
Catherine L. Farage
Keyword(s):  
Spiral Galaxy ◽  
Near Infrared ◽  
Infrared Imaging ◽  
Star Formation History ◽  
Star Forming ◽  
Star Forming Regions ◽  
The North ◽  
Contact Points ◽  
Nuclear Ring ◽  
Barred Spiral Galaxy

AbstractWe present infrared imaging from IRIS2 on the Anglo–Australian Telescope that shows the barred spiral galaxy IC 4933 has not just an inner ring encircling the bar, but also a star-forming nuclear ring 1.5 kpc in diameter. Imaging in the u′ band with GMOS on Gemini South confirms that this ring is not purely an artifact due to dust. Optical and near-infrared colours alone however cannot break the degeneracy between age, extinction, and burst duration that would allow the star formation history of the ring to be unraveled. Integral field spectroscopy with the GNIRS spectrograph on Gemini South shows the equivalent width of the Paβ line to peak in the north and south quadrants of the ring, indicative of a bipolar azimuthal age gradient around the ring. The youngest star-forming regions do not appear to correspond to where we expect to find the contact points between the offset dust lanes and the nuclear ring unless the nuclear ring is oval in shape, causing the contact points to lead the bar by more than 90°.

scholarly journals Ionized and neutral gas in the XUV discs of nearby spiral galaxies

2014 ◽  
Vol 10 (S309) ◽  
pp. 65-68
Author(s):  
López-Sánchez ◽  
B. S. Koribalski ◽  
T. Westmeier ◽  
C. Esteban
Keyword(s):  
Spiral Galaxies ◽  
Dwarf Galaxy ◽  
Chemical Abundances ◽  
Ionized Gas ◽  
Galaxy Interactions ◽  
Star Forming ◽  
Star Forming Regions ◽  
Neutral Gas ◽  
The Galaxy ◽  
Nearby Galaxies

AbstractWe are conducting a multiwavelength study of XUV discs in nearby, gas-rich spiral galaxies combining the available UV (GALEX) observations with H i data obtained at the ATCA as part of the Local Volume HI Survey (LVHIS) project and multi-object fibre spectroscopy obtained using the 2dF/AAOmega instrument at the 3.9m AAT. Here we present the results of the multiwavelength analysis of the galaxy pair NGC 1512/1510. The H i distribution of NGC 1512 is very extended with two pronounced spiral/tidal arms. Hundreds of independent UV-bright regions are associated with dense H i clouds in the galaxy outskirts. We confirm the detection of ionized gas in the majority of them and characterize their physical properties, chemical abundances and kinematics. Both the gas distribution andthe distribution of the star-forming regions are affected by gravitational interactionwith the neighbouring blue compact dwarf galaxy NGC 1510. Our multiwavelength analysis provides new clues about local star-formation processes, the metal redistribution in the outer gaseous discs of spiral galaxies, the importance of galaxy interactions, the fate of the neutral gas and the chemical evolution in nearby galaxies.

scholarly journals Star forming regions in a sample of HST spiral galaxies

2013 ◽  
Vol 553 ◽  
pp. A87 ◽  
Author(s):  
P. Drazinos ◽  
E. Kontizas ◽  
A. Karampelas ◽  
M. Kontizas ◽  
A. Dapergolas
Keyword(s):  
Spiral Galaxies ◽  
Star Forming ◽  
Star Forming Regions

scholarly journals Study photometric properties of spiral galaxy NGC 4448 using CCD camera with multiband filters

2018 ◽  
Vol 15 (35) ◽  
pp. 8-13
Author(s):  
Sinan H. Ali
Keyword(s):  
Spiral Galaxy ◽  
Surface Brightness ◽  
Galactic Center ◽  
Ccd Camera ◽  
Position Angle ◽  
Ccd Photometry ◽  
Optical Telescope ◽  
Star Forming ◽  
Star Forming Regions ◽  
The Galaxy

The goal of our study is to perform detailed multiband surface photometry of the spiral galaxy NGC 4448 and its brightest star-forming regions. The structure and composition of the stellar population in the surface brightness galaxy NGC 4448 was studied using BVR CCD photometry. The observations were obtained on the 1.88 m optical telescope of Kottamia Astronomical Observatory (KAO), Egypt. A two-dimensional decomposition of the galaxy bulge and disk components is carried out. A powerful star forming region is observed near the galactic center. Based on the positions of the various components of the galaxy in two color diagrams. From the observations, the surface brightness profiles, Ellipticity profiles, position angle profiles and color indices profiles are described and studied.

scholarly journals Analysis of VLBI Spot Map of H20 Masers for the HII Region Complex IC133 of Spiral Galaxy M33

1996 ◽  
Vol 175 ◽  
pp. 181-182
Author(s):  
Yu Zhi-Yao
Keyword(s):  
Spiral Galaxy ◽  
Spectral Feature ◽  
Hii Region ◽  
Active Star ◽  
Star Forming ◽  
Star Forming Regions ◽  
Peak Flux ◽  
The Galaxy ◽  
Distinct Features ◽  
Maser Sources

Interstellar H2O masers in the Galaxy occur in active star forming regions. The spectrum often shows multiple distinct features. The VLBI maps reveal that each spectral feature corresponds to emission of spatially distinct maser sources (maser spots), whose sizes are ≈ 1013cm. The maser in M33 is associated with the HII region complex IC133, which has been studied optically by Boulesteix et al. (1974) and Kiwitter and Aller (1981). This maser is the nearest (≤ 1Mpc) extragalactic H2O source visible in the northern sky, although it is not the strongest. It is known to have persisted for over a decade, and its spectra consistently show peak flux densities of ≈ 1.5 Jy and at least 10 features spread over ≈ 50 km s–1 (Huchtmeier, Eckart and Zensus 1988). Using VLBI Greehill et al. (1990) have obtained the positions of 14 H2O maser spots.

scholarly journals Cosmological simulations of the same spiral galaxy: the impact of baryonic physics

2020 ◽  
Vol 501 (1) ◽  
pp. 62-77
Author(s):  
A Nuñez-Castiñeyra ◽  
E Nezri ◽  
J Devriendt ◽  
R Teyssier
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Galaxy Formation ◽  
Spiral Galaxy ◽  
Milky Way ◽  
Spiral Galaxies ◽  
Cosmological Simulations ◽  
Star Forming ◽  
Small Scales ◽  
The Impact

ABSTRACT The interplay of star formation (SF) and supernova (SN) feedback in galaxy formation is a key element for understanding galaxy evolution. Since these processes occur at small scales, it is necessary to have sub-grid models that recover their evolution and environmental effects at the scales reached by cosmological simulations. In this work, we present the results of the Mochima simulation, where we simulate the same spiral galaxy inhabiting a Milky Way (MW) size halo in a cosmological environment changing the sub-grid models for SN feedback and SF. We test combinations of the Schmidt law and a multifreefall based SF with delayed cooling feedback or mechanical feedback. We reach a resolution of 35 pc in a zoom-in box of 36 Mpc. For this, we use the code $\rm{\small RAMSES}$ with the implementation of gas turbulence in time and trace the local hydrodynamical features of the star-forming gas. Finally, we compare the galaxies at redshift 0 with global and interstellar medium observations in the MW and local spiral galaxies. The simulations show successful comparisons with observations. Nevertheless, diverse galactic morphologies are obtained from different numerical implementations. We highlight the importance of detailed modelling of the SF and feedback processes, especially for simulations with a resolution that start to reach scales relevant for molecular cloud physics. Future improvements could alleviate the degeneracies exhibited in our simulated galaxies under different sub-grid models.

Sign in / Sign up

Export Citation Format

Share Document