Where stars form: inside-out growth and coherent star formation from
... scaffolding of this project upon which all the remaining data products rest. For this study, we rely on the rest-frame colors, stellar masses, and star formation rates. All of these quantities were derived based on constraints from across the electromagnetic spectrum. Our redshift fitting method als ...
... scaffolding of this project upon which all the remaining data products rest. For this study, we rely on the rest-frame colors, stellar masses, and star formation rates. All of these quantities were derived based on constraints from across the electromagnetic spectrum. Our redshift fitting method als ...
2. The X-ray-Radio correlation for bulgeless galaxies
... evolution of massive stars and their destruction, suggesting the possibility of using X-ray emission to determine the star formation rates. This work presents a study on the presence of this correlation in bulgeless galaxies at intermediate redshifts ( 0.4≤z≤1.0 ). To this effect, the VLA and Chandr ...
... evolution of massive stars and their destruction, suggesting the possibility of using X-ray emission to determine the star formation rates. This work presents a study on the presence of this correlation in bulgeless galaxies at intermediate redshifts ( 0.4≤z≤1.0 ). To this effect, the VLA and Chandr ...
Probing nuclear activity versus star formation at z ∼ 0.8 using near
... The latter authors found that the period of moderately luminous AGN activity does not seem to have strong influence on the star formation activity of the galaxies, in contradiction with the results found at low redshift (e.g. Ho 2005). For example, based on FIR data from the Herschel Space Observato ...
... The latter authors found that the period of moderately luminous AGN activity does not seem to have strong influence on the star formation activity of the galaxies, in contradiction with the results found at low redshift (e.g. Ho 2005). For example, based on FIR data from the Herschel Space Observato ...
Chapter 24
... rich in interstellar matter and young, blue stars, but they lack any regular structure, such as well-defined spiral arms or central bulges. They are divided into two subclasses: Irr I galaxies and Irr II galaxies. The Irr I galaxies often look like misshapen spirals. Irregular galaxies tend to be sm ...
... rich in interstellar matter and young, blue stars, but they lack any regular structure, such as well-defined spiral arms or central bulges. They are divided into two subclasses: Irr I galaxies and Irr II galaxies. The Irr I galaxies often look like misshapen spirals. Irregular galaxies tend to be sm ...
Revising the census of low luminosity AGN
... ONLY A FEW PERCENT! MOST OF THEM HAVE LOW EW AND ARE UNLIKELY TO BE AGN THE LINE EMISSION IS PRODUCED BY THE HOST GALAXY, NOT BY THE AGN THE LINERs REGION IS MOSTLY POPULATED BY NON-AGN THE EW IS A BEST PREDICTOR FOR GENUINE AGN THAN THE DIAGNOSTIC DIAGRAMS A LOW EW (~1 Å) IS CHARACTERISTIC OF STELL ...
... ONLY A FEW PERCENT! MOST OF THEM HAVE LOW EW AND ARE UNLIKELY TO BE AGN THE LINE EMISSION IS PRODUCED BY THE HOST GALAXY, NOT BY THE AGN THE LINERs REGION IS MOSTLY POPULATED BY NON-AGN THE EW IS A BEST PREDICTOR FOR GENUINE AGN THAN THE DIAGNOSTIC DIAGRAMS A LOW EW (~1 Å) IS CHARACTERISTIC OF STELL ...
SPICA Yellow Book
... A selection of the fine-structure atomic and ionic lines accessible with SPICA, plotted as a function of critical density and ionisation potential. Using ratios between lines with different ionisation or critical densities, we can trace out a wide range of different physical-excitation conditions (S ...
... A selection of the fine-structure atomic and ionic lines accessible with SPICA, plotted as a function of critical density and ionisation potential. Using ratios between lines with different ionisation or critical densities, we can trace out a wide range of different physical-excitation conditions (S ...
THE STAR FORMATION AND NUCLEAR ACCRETION HISTORIES OF NORMAL GALAXIES
... may be most abundant at z < ∼ 1 and, if so, they could produce a substantial fraction of the “normal” galaxy X-ray flux at these redshifts. Given their similar evolution, spectral shapes (e.g., Ptak et al. 1999), and potentially similar luminosities, it may be difficult to disentangle the X-ray emis ...
... may be most abundant at z < ∼ 1 and, if so, they could produce a substantial fraction of the “normal” galaxy X-ray flux at these redshifts. Given their similar evolution, spectral shapes (e.g., Ptak et al. 1999), and potentially similar luminosities, it may be difficult to disentangle the X-ray emis ...
Elliptical Galaxies
... center of a galaxy an increase in dispersion may indicate an increase in M/L or an increase in the fraction of radial orbits. The latter will, however, produce a line profile that is less sharply peaked than a Gaussian. Thus by measuring deviations from a Gaussian profile as well as its width we can ...
... center of a galaxy an increase in dispersion may indicate an increase in M/L or an increase in the fraction of radial orbits. The latter will, however, produce a line profile that is less sharply peaked than a Gaussian. Thus by measuring deviations from a Gaussian profile as well as its width we can ...
Lab 14 Galaxy Morphology
... Figure 14.11: An irregular galaxy that is the result of the collision between two galaxies. The larger galaxy appears to have once been a normal spiral galaxy. But another galaxy (visible in the bottom right corner) ran into the bigger galaxy, and destroyed the symmetry typically found in a spiral ...
... Figure 14.11: An irregular galaxy that is the result of the collision between two galaxies. The larger galaxy appears to have once been a normal spiral galaxy. But another galaxy (visible in the bottom right corner) ran into the bigger galaxy, and destroyed the symmetry typically found in a spiral ...
– 1 – 1. Galaxy Observations 1.1.
... rate affecting the UV continuum, and the calibration for UV stellar photospheric features or UV ISM absorption to metallicity is not well understood at present (see Erb 2010 for details). So the best approach is to move into the near-IR, where the normal optical low redshift techniques and calibrati ...
... rate affecting the UV continuum, and the calibration for UV stellar photospheric features or UV ISM absorption to metallicity is not well understood at present (see Erb 2010 for details). So the best approach is to move into the near-IR, where the normal optical low redshift techniques and calibrati ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... our own. These nearby systems also provide our clearest views of how galaxies interact with one another in the relatively small volume of space of the Local Group. The brightest members of the Local Group are so close to us that on a clear, dark night away from city lights it is possible to see them ...
... our own. These nearby systems also provide our clearest views of how galaxies interact with one another in the relatively small volume of space of the Local Group. The brightest members of the Local Group are so close to us that on a clear, dark night away from city lights it is possible to see them ...
Far-ultraviolet and far-infrared bivariate luminosity function of galaxies:
... star formation rate (hereafter SFR) has been of central importance to an understanding of the formation and evolution of galaxies. However, this has been a difficult task for a long time because of dust extinction. Active star formation (SF) is always accompanied by dust production through various d ...
... star formation rate (hereafter SFR) has been of central importance to an understanding of the formation and evolution of galaxies. However, this has been a difficult task for a long time because of dust extinction. Active star formation (SF) is always accompanied by dust production through various d ...
Hubble Space Telescope Imaging of Post
... responsible for the formation of large (i.e., elliptical) galaxies via mergers of smaller (e.g., spiral) systems (Toomre 1977). Ultraluminous infrared galaxies (ULIRGs), interacting systems powered by both starburst and active galactic nuclei (AGN), have been hypothesized to evolve into “normal” (i. ...
... responsible for the formation of large (i.e., elliptical) galaxies via mergers of smaller (e.g., spiral) systems (Toomre 1977). Ultraluminous infrared galaxies (ULIRGs), interacting systems powered by both starburst and active galactic nuclei (AGN), have been hypothesized to evolve into “normal” (i. ...
EROs and submm galaxies: Expectations for FMOS in the
... been resolved into submillimetre galaxies (SMGs) which appear to be dusty vigorous star-forming galaxies. Half the total extragalactic background is in the submm, while SMGs make up more than half the extragalactic submm background >25% of all stars since the Big Bang have formed in SMGs. ...
... been resolved into submillimetre galaxies (SMGs) which appear to be dusty vigorous star-forming galaxies. Half the total extragalactic background is in the submm, while SMGs make up more than half the extragalactic submm background >25% of all stars since the Big Bang have formed in SMGs. ...
lecture course
... In most galaxy samples there are roughly equal numbers of elliptical, spiral, and peculiar (irregular) galaxies. Elliptical galaxies come in two types - giant ellipticals, which have high brightnesses at their centres and absolute B magnitudes between about -25 and -15, and dwarf ellipticals, which ...
... In most galaxy samples there are roughly equal numbers of elliptical, spiral, and peculiar (irregular) galaxies. Elliptical galaxies come in two types - giant ellipticals, which have high brightnesses at their centres and absolute B magnitudes between about -25 and -15, and dwarf ellipticals, which ...
The environment of high-redshift AGN OLIMPIA JUDIT FOGASY
... 1967; Steidel et al. 1995). As young stars emit mostly UV light and photons with energies higher than the ionization energy of hydrogen are easily absorbed by neutral gas around star-forming regions, a break can be observed in the spectral energy distribution (SED) of the galaxy at 91.2 nm rest-fram ...
... 1967; Steidel et al. 1995). As young stars emit mostly UV light and photons with energies higher than the ionization energy of hydrogen are easily absorbed by neutral gas around star-forming regions, a break can be observed in the spectral energy distribution (SED) of the galaxy at 91.2 nm rest-fram ...
Introduction
... a dataset of multiwavelength observations for a new sample of galaxies. The sample is volume and mass limited, and includes galaxies of all morphological types inhabiting a range of different environments, from galaxies in the dense core of the Virgo cluster to relatively isolated systems. As such, ...
... a dataset of multiwavelength observations for a new sample of galaxies. The sample is volume and mass limited, and includes galaxies of all morphological types inhabiting a range of different environments, from galaxies in the dense core of the Virgo cluster to relatively isolated systems. As such, ...
Lecture 2
... • “low-excitation lines will map out a larger fraction of the ISM in these galaxies and…study in detail the spacially resolved kinematic structure of most of the gas…which resides in the cold phase” (Carilli & Blain ...
... • “low-excitation lines will map out a larger fraction of the ISM in these galaxies and…study in detail the spacially resolved kinematic structure of most of the gas…which resides in the cold phase” (Carilli & Blain ...
Galaxies
... The radiation from these galaxies is called nonstellar radiation Many luminous galaxies are experiencing an outburst of star formation, probably due to interactions with a neighbor These galaxies are called starburst galaxies, and we will discuss them later The galaxies we will discuss now are those ...
... The radiation from these galaxies is called nonstellar radiation Many luminous galaxies are experiencing an outburst of star formation, probably due to interactions with a neighbor These galaxies are called starburst galaxies, and we will discuss them later The galaxies we will discuss now are those ...
Super-solar Metal Abundances in Two Galaxies at ζ ∼ 3.57
... 2008; Mannucci et al. 2009). The emerging picture is that the spread in metallicity is large at any redshift, certainly much larger than what one would expect based on DLAs in QSO spectra alone. DLAs are regularly detected in spectra of gamma-ray burst (GRB) afterglows. Long GRBs are the most lumino ...
... 2008; Mannucci et al. 2009). The emerging picture is that the spread in metallicity is large at any redshift, certainly much larger than what one would expect based on DLAs in QSO spectra alone. DLAs are regularly detected in spectra of gamma-ray burst (GRB) afterglows. Long GRBs are the most lumino ...
– 1 – 1. Emission Lines in Nearby Galaxies 1.1.
... de-excitation can be ignored. This results in an overpopulation of the metastable states and the forbidden transitions dominate the spectrum. If one can find a single ion with two or more detectable forbidden lines arising from very different excitation energy levels, the ratio of their strengths wi ...
... de-excitation can be ignored. This results in an overpopulation of the metastable states and the forbidden transitions dominate the spectrum. If one can find a single ion with two or more detectable forbidden lines arising from very different excitation energy levels, the ratio of their strengths wi ...
PDF only - at www.arxiv.org.
... vertical H2O2 profiles and in a unique way constrain photochemical models. Other important species are HO2 and OH not observed by HIFI, since Mars’ apparent diameter was too small during the Herschel observation windows so that the planet was not resolved. With larger collection area and higher s ...
... vertical H2O2 profiles and in a unique way constrain photochemical models. Other important species are HO2 and OH not observed by HIFI, since Mars’ apparent diameter was too small during the Herschel observation windows so that the planet was not resolved. With larger collection area and higher s ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... contribute very little to the luminosity of the event. This is because high-mass stars are much more luminous than low-mass ones. A star of 100 M is about 1000 000 times brighter than the Sun. Even if there is only one star of 100 M every 500 stars of 1 M , it alone outshines all of them, whose c ...
... contribute very little to the luminosity of the event. This is because high-mass stars are much more luminous than low-mass ones. A star of 100 M is about 1000 000 times brighter than the Sun. Even if there is only one star of 100 M every 500 stars of 1 M , it alone outshines all of them, whose c ...
Galaxy Evolution
... contribute very little to the luminosity of the event. This is because high-mass stars are much more luminous than low-mass ones. A star of 100 M is about 1000 000 times brighter than the Sun. Even if there is only one star of 100 M every 500 stars of 1 M , it alone outshines all of them, whose c ...
... contribute very little to the luminosity of the event. This is because high-mass stars are much more luminous than low-mass ones. A star of 100 M is about 1000 000 times brighter than the Sun. Even if there is only one star of 100 M every 500 stars of 1 M , it alone outshines all of them, whose c ...
Megamaser
A megamaser is a type of astrophysical maser, which is a naturally occurring source of stimulated spectral line emission. Megamasers are distinguished from astrophysical masers by their large isotropic luminosity. Megamasers have typical luminosities of 103 solar luminosities (L☉), which is 100 million times brighter than masers in the Milky Way, hence the prefix mega. Likewise, the term kilomaser is used to describe masers outside the Milky Way that have luminosities of order L☉, or thousands of times stronger than the average maser in the Milky Way, gigamaser is used to describe masers billions of times stronger than the average maser in the Milky Way, and extragalactic maser encompasses all masers found outside the Milky Way. Most known extragalactic masers are megamasers, and the majority of megamasers are hydroxyl (OH) megamasers, meaning the spectral line being amplified is one due to a transition in the hydroxyl molecule. There are known megamasers for three other molecules: water (H2O), formaldehyde (H2CO), and methine (CH).Water megamasers were the first type of megamaser discovered. The first water megamaser was found in 1979 in NGC 4945, a galaxy in the nearby Centaurus A/M83 Group. The first hydroxyl megamaser was found in 1982 in Arp 220, which is the nearest ultraluminous infrared galaxy to the Milky Way. All subsequent OH megamasers that have been discovered are also in luminous infrared galaxies, and there are a small number of OH kilomasers hosted in galaxies with lower infrared luminosities. Most luminous infrared galaxies have recently merged or interacted with another galaxy, and are undergoing a burst of star formation. Many of the characteristics of the emission in hydroxyl megamasers are distinct from that of hydroxyl masers within the Milky Way, including the amplification of background radiation and the ratio of hydroxyl lines at different frequencies. The population inversion in hydroxyl molecules is produced by far infrared radiation that results from absorption and re-emission of light from forming stars by surrounding interstellar dust. Zeeman splitting of hydroxyl megamaser lines may be used to measure magnetic fields in the masing regions, and this application represents the first detection of Zeeman splitting in a galaxy other than the Milky Way.Water megamasers and kilomasers are found primarily associated with active galactic nuclei, while galactic and weaker extragalactic water masers are found in star forming regions. Despite different environments, the circumstances that produce extragalactic water masers do not seem to be very different from those that produce galactic water masers. Observations of water megamasers have been used to make accurate measurements of distances to galaxies in order to provide constraints on the Hubble constant.