scholarly journals The Integral Field View of the Orion Nebula

2014 ◽  
Vol 2014 ◽  
pp. 1-14
Author(s):  
Adal Mesa-Delgado
Keyword(s):  
Large Scale ◽  
3D Structure ◽  
Active Role ◽  
Small Scale ◽  
H Ii Regions ◽  
Orion Nebula ◽  
Star Forming ◽  
Star Forming Regions ◽  
Integral Field Spectroscopy ◽  
Integral Field

This paper reviews the major advances achieved in the Orion Nebula through the use of integral field spectroscopy (IFS). Since the early work of Vasconcelos and collaborators in 2005, this technique has facilitated the investigation of global properties of the nebula and its morphology, providing new clues to better constrain its 3D structure. IFS has led to the discovery of shock-heated zones at the leading working surfaces of prominent Herbig-Haro objects as well as the first attempt to determine the chemical composition of Orion protoplanetary disks, also known asproplyds. The analysis of these morphologies using IFS has given us new insights into the abundance discrepancy problem, a long-standing and unresolved issue that casts doubt on the reliability of current methods used for the determination of metallicities in the universe from the analysis of H II regions. Results imply that high-density clumps and high-velocity flows may play an active role in the production of such discrepancies. Future investigations based on the large-scale IFS mosaic of Orion will be very valuable for exploring how the integrated effect of small-scale structures may have impact at larger scales in the framework of star-forming regions.

scholarly journals A geostatistical analysis of multiscale metallicity variations in galaxies [I]: Introduction and comparison of high-resolution metallicity maps to an analytic metal transport model

2021 ◽  
Author(s):  
Benjamin Metha ◽  
Michele Trenti ◽  
Tingjin Chu
Keyword(s):  
Large Scale ◽  
Transport Model ◽  
Small Scale ◽  
H Ii Regions ◽  
Integral Field Spectroscopy ◽  
Physical Scale ◽  
Interstellar Media ◽  
Nearby Galaxies ◽  
The Mean ◽  
Linear Regressions

Abstract Thanks to recent advances in integral field spectroscopy (IFS), modern surveys of nearby galaxies are capable of resolving metallicity maps of H ii regions down to scales of ∼50pc. However, statistical analysis of these metallicity maps has seldom gone beyond fitting basic linear regressions and comparing parameters to global galaxy properties. In this paper (the first of a series), we introduce techniques from spatial statistics that are well suited for detailed analysis of both small- and large-scale metallicity variations within the interstellar media (ISMs) of local galaxies. As a first application, we compare the observed structure of small-scale metallicity fluctuations within 7 local galaxies observed by the PHANGS collaboration to predictions from a stochastic, physically motivated, analytical model developed by Krumholz & Ting. We show that while the theoretical model underestimates the amount of correlated scatter in the galactic metallicity distributions by 3 − 4 orders of magnitude, it provides good estimates of the physical scale of metallicity correlations. We conclude that the ISM of local spiral galaxies is far from homogeneous, with regions of size ∼1 kpc showing significant departures from the mean metallicity at each galactocentric radius.

scholarly journals Intense velocity-shears and magnetic fields in diffuse molecular gas: from 10 pc to 5 mpc

2009 ◽  
Vol 5 (H15) ◽  
pp. 442-443
Author(s):  
Edith Falgarone ◽  
Pierre Hily-Blant
Keyword(s):  
Velocity Field ◽  
Magnetic Fields ◽  
Large Scale ◽  
Dust Emission ◽  
Large Scale Structure ◽  
Small Scale ◽  
Molecular Gas ◽  
Gas Velocity ◽  
Star Forming ◽  
Star Forming Regions

AbstractRegions of intense velocity-shears are identified on statistical grounds in nearby diffuse molecular gas: they form conspicuous thin (~ 0.03 pc) and parsec-long structures that do not bear the signatures of shocked gas. Several straight substructures, ~ 3 mpc thick, have been detected at different position-angles within one of them. Two exhibit the largest velocity-shears ever measured far from star forming regions, up to 780 kms−1pc−1. Their position-angles are found to be also those of 10-parsec striations in the I(100μm) dust emission of the large scale environment. The B field projections, where available in these fields, are parallel both to the parsec- and to one of the milliparsec-scale shears. These findings put in relation the small-scale intermittent facet of the gas velocity field and the large scale structure of the magnetic fields.

scholarly journals Inner and outer star forming regions over the disks of spiral galaxies

2018 ◽  
Vol 609 ◽  
pp. A102 ◽  
Author(s):  
M. Rodríguez-Baras ◽  
A. I. Díaz ◽  
F. F. Rosales-Ortega ◽  
S. F. Sánchez
Keyword(s):  
Galaxy Formation ◽  
Spiral Galaxies ◽  
Complete Characterization ◽  
Star Forming ◽  
Star Forming Regions ◽  
Integral Field Spectroscopy ◽  
Formation And Evolution ◽  
Inside Out ◽  
Integral Field

Context. The knowledge of abundance distributions is central to understanding the formation and evolution of galaxies. Most of the relations employed for the derivation of gas abundances have so far been derived from observations of outer disk H ii regions, despite the known differences between inner and outer regions. Aims. Using integral field spectroscopy (IFS) observations we aim to perform a systematic study and comparison of two inner and outer H ii regions samples. The spatial resolution of the IFS, the number of objects and the homogeneity and coherence of the observations allow a complete characterization of the main observational properties and differences of the regions. Methods. We analyzed a sample of 725 inner H ii regions and a sample of 671 outer H ii regions, all of them detected and extracted from the observations of a sample of 263 nearby, isolated, spiral galaxies observed by the CALIFA survey. Results. We find that inner H ii regions show smaller equivalent widths, greater extinction and luminosities, along with greater values of [N ii] λ6583/Hα and [O ii] λ3727/[O iii] λ5007 emission-line ratios, indicating higher metallicities and lower ionization parameters. Inner regions have also redder colors and higher photometric and ionizing masses, although Mion/Mphot is slighty higher for the outer regions. Conclusions. This work shows important observational differences between inner and outer H ii regions in star forming galaxies not previously studied in detail. These differences indicate that inner regions have more evolved stellar populations and are in a later evolution state with respect to outer regions, which goes in line with the inside-out galaxy formation paradigm.

scholarly journals Large-scale [C II] 158 μm emission from the Orion-Eridanus superbubble

2020 ◽  
Vol 639 ◽  
pp. A110
Author(s):  
A. Abdullah ◽  
A. G. G. M. Tielens
Keyword(s):  
Molecular Clouds ◽  
Large Scale ◽  
Substantial Contribution ◽  
Small Scale ◽  
Neutral Medium ◽  
Ionized Gas ◽  
Star Forming ◽  
Radiation Fields ◽  
Star Forming Regions ◽  
Warm Ionized Medium

In this study, we analyzed the [C II] 158 μm emission from the Orion-Eridanus region measured by the Cosmic Background Explorer. Morphologically, the [C II] emission traces prominent star-forming regions this area. The analysis takes into account five different components of the interstellar medium (ISM) that can contribute to the [C II] emission: compact H II regions, dense Photon-Dominated Region, surfaces of molecular clouds, the Warm Ionized Medium, and the Cold Neutral Medium. We estimate the contribution from each object of interest to the observed [C II] emission based upon the physical properties of the object and validate our results by making a comparison with existing “small” scale maps. Inside the ~400 parsec aperture radius that we investigate, surfaces of molecular clouds exposed to radiation from nearby stellar clusters are the dominant contributor to the observed global [C II] flux. These molecular cloud surfaces are exposed to moderate radiation fields (G0 ~ 100 times the average interstellar radiation field) and are moderately dense (nH ~ 103 cm−3). In addition, extended low-density ionized gas, along with large-scale ionized gas structures (Barnard’s Loop; λ Ori) also make a substantial contribution. The implications of this study for the analysis of extragalactic [C II] observations are assessed.

scholarly journals Inner and outer star forming regions over the discs of spiral galaxies I. Sample characterization

2016 ◽  
Vol 11 (S321) ◽  
pp. 296-296
Author(s):  
Marina Rodríguez-Baras ◽  
A.I. Díaz ◽  
F.F. Rosales-Ortega
Keyword(s):  
Star Formation ◽  
Disk Galaxies ◽  
Work Sample ◽  
Star Forming ◽  
Star Forming Regions ◽  
Integral Field Spectroscopy ◽  
The Galaxy ◽  
Sample Characterization ◽  
Integral Field

AbstractThis project is aimed at understanding the dependence of star formation on the environment by analysing young stellar populations in two very different positions in disk galaxies: circumnuclear and outer disk giant regions. Integral field spectroscopy (IFS) provide an ideal means to achieve these goals providing simultaneous spatial and spectral resolution. Here we present the characterization of the work sample, composed by 671 outer regions and 725 inner regions from 263 isolated spirals galaxies observed by the CALIFA survey. The wide number of regions in both samples allows us to obtain statistically relevant results about the influence of metallicity, density and environment on star formation, and how it disseminates over the galaxy, to obtain evolutionary stories for the star-forming regions and to compare our results with models of massive star formation and galactic chemical evolution.

scholarly journals Mapping the Dynamics of the Quasar 3C 48

2001 ◽  
Vol 205 ◽  
pp. 162-165
Author(s):  
Eleni T. Chatzichristou
Keyword(s):  
Emission Line ◽  
Radio Source ◽  
Star Forming ◽  
Physical Conditions ◽  
Star Forming Regions ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Ir Emission ◽  
Integral Field ◽  
Extended Emission

The archetypical, nearby (z=0.37) quasar 3C 48 is an unusual CSS radio source with excess far-IR emission, whose one-sided radio jet is aligned with the extended ionized emission and a putative second nucleus. Because of its high AGN luminosity and proximity, 3C 48 is a good candidate to search for kinematic signatures of the radio jet-gas coupling and/or of a recent interaction. The radio morphology and our ground-based integral field spectroscopy suggest that the jet is interacting with its immediate environment. Using STIS aboard HST in several slit positions within the central 1”, we map the kinematics and physical conditions of the extended emission line gas and their relations to near-nuclear star forming regions found in existing HST images.

IRX–βRELATION OF STAR-FORMING REGIONS IN NGC 628 BASED ON INTEGRAL FIELD SPECTROSCOPY

2016 ◽  
Vol 826 (2) ◽  
pp. 209 ◽  
Author(s):  
Chengyun Ye ◽  
Hu Zou ◽  
Lin Lin ◽  
Jianhui Lian ◽  
Ning Hu ◽  
...  
Keyword(s):  
Star Forming ◽  
Star Forming Regions ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field

scholarly journals Integral field spectroscopy of local LCBGs: NGC 7673, a case study. Physical properties of star-forming regions

2010 ◽  
Vol 411 (3) ◽  
pp. 1819-1832 ◽  
Author(s):  
A. Castillo-Morales ◽  
J. Gallego ◽  
J. Pérez-Gallego ◽  
R. Guzmán ◽  
J. C. Muñoz-Mateos ◽  
...  
Keyword(s):  
Physical Properties ◽  
Star Forming ◽  
Star Forming Regions ◽  
Integral Field Spectroscopy ◽  
Field Spectroscopy ◽  
Integral Field

scholarly journals Double trouble: Gaia reveals (proto)planetary systems that may experience more than one dense star-forming environment

2020 ◽  
Vol 501 (1) ◽  
pp. L12-L17
Author(s):  
Christina Schoettler ◽  
Richard J Parker
Keyword(s):  
Planetary Systems ◽  
Young Star ◽  
Young Stars ◽  
Orion Nebula ◽  
External Effects ◽  
Star Forming ◽  
Star Forming Regions ◽  
Ejection Process ◽  
Runaway Stars

ABSTRACT Planetary systems appear to form contemporaneously around young stars within young star-forming regions. Within these environments, the chances of survival, as well as the long-term evolution of these systems, are influenced by factors such as dynamical interactions with other stars and photoevaporation from massive stars. These interactions can also cause young stars to be ejected from their birth regions and become runaways. We present examples of such runaway stars in the vicinity of the Orion Nebula Cluster (ONC) found in Gaia DR2 data that have retained their discs during the ejection process. Once set on their path, these runaways usually do not encounter any other dense regions that could endanger the survival of their discs or young planetary systems. However, we show that it is possible for star–disc systems, presumably ejected from one dense star-forming region, to encounter a second dense region, in our case the ONC. While the interactions of the ejected star–disc systems in the second region are unlikely to be the same as in their birth region, a second encounter will increase the risk to the disc or planetary system from malign external effects.

The DIVING3D Project: Analysis of the nuclear region of Early-type Galaxies

2020 ◽  
Vol 15 (S359) ◽  
pp. 454-456
Author(s):  
T. V. Ricci ◽  
J. E. Steiner ◽  
R. B. Menezes
Keyword(s):  
Emission Lines ◽  
H Ii Regions ◽  
Sample Type ◽  
Early Type ◽  
Integral Field Spectroscopy ◽  
Project Analysis ◽  
Line Region ◽  
Field Unit ◽  
Integral Field

AbstractIn this work, we present preliminary results regarding the nuclear emission lines of a statistically complete sample of 56 early-type galaxies that are part of the Deep Integral Field Spectroscopy View of Nuclei of Galaxies (DIVING3D) Project. All early type galaxies (ETGs) were observed with the Gemini Multi-Object Spectrograph Integral Field Unit (GMOS-IFU) installed on the Gemini South Telescope. We detected emission lines in 93% of the sample, mostly low-ionization nuclear emission-line region galaxies (LINERs). We did not find Transition Objects nor H II regions in the sample. Type 1 objects are seen in ∼23% of the galaxies.

Sign in / Sign up

Export Citation Format

Share Document