N-Body/SPH simulations of induced star formation in dwarf galaxies
... out that dark matter is necessary to explain large scale structure formation and the origin of galaxies. Structure in the universe is believed to originate hierarchically. Primarily, small density perturbations arise. Pressureless dark matter clumps together in these density perturbations and dark m ...
... out that dark matter is necessary to explain large scale structure formation and the origin of galaxies. Structure in the universe is believed to originate hierarchically. Primarily, small density perturbations arise. Pressureless dark matter clumps together in these density perturbations and dark m ...
Hubble 2006: Science Year in Review
... The servicing mission in 1999 enhanced many of Hubble’s subsystems, including the central computer, a new solid-state data-recording system to replace the aging magnetic tape drives, and the gyroscopes needed for pointing control. A month prior to launch, a gyroscope failure had forced Hubble into ...
... The servicing mission in 1999 enhanced many of Hubble’s subsystems, including the central computer, a new solid-state data-recording system to replace the aging magnetic tape drives, and the gyroscopes needed for pointing control. A month prior to launch, a gyroscope failure had forced Hubble into ...
The Evolution of Star Formation Activity in . Cory R. Wagner
... substantial dust-obscured star formation activity (Hilton et al. 2010; Tran et al. 2010; Santos et al. 2013; Brodwin et al. 2013, hereafter B13). Alberts et al. (2014, hereafter A14) found that dust-obscured star formation in cluster galaxies increases with lookback time from z = 0.3 → 1.5. Several ...
... substantial dust-obscured star formation activity (Hilton et al. 2010; Tran et al. 2010; Santos et al. 2013; Brodwin et al. 2013, hereafter B13). Alberts et al. (2014, hereafter A14) found that dust-obscured star formation in cluster galaxies increases with lookback time from z = 0.3 → 1.5. Several ...
The correlation between galaxy morphology and star
... activity (z ∼ 2 − 3). Until relatively recently, most studies of galaxy morphologies at z > 2 have been performed at rest–frame ultraviolet (UV) wavelengths using optical imagers (such as HST/WFPC2 and HST/ACS). These works found that irregular or peculiar structures appear more common, and traditio ...
... activity (z ∼ 2 − 3). Until relatively recently, most studies of galaxy morphologies at z > 2 have been performed at rest–frame ultraviolet (UV) wavelengths using optical imagers (such as HST/WFPC2 and HST/ACS). These works found that irregular or peculiar structures appear more common, and traditio ...
THE UV-OPTICAL COLOR MAGNITUDE DIAGRAM. II. PHYSICAL
... We use the UV-optical color magnitude diagram in combination with spectroscopic and photometric measurements derived from the SDSS spectroscopic sample to measure the distribution of galaxies in the local universe (z < 0:25) and their physical properties as a function of specific star formation rate ...
... We use the UV-optical color magnitude diagram in combination with spectroscopic and photometric measurements derived from the SDSS spectroscopic sample to measure the distribution of galaxies in the local universe (z < 0:25) and their physical properties as a function of specific star formation rate ...
Physics of the Interstellar Medium
... enormous interest and that made ISM physics a major astrophysical research topic, not only in Germany but worldwide. Recently, tremendous progress has been made in identifying the various processes that shape the ISM. It has become clear that its non-linear dynamics and multi-scale structure require ...
... enormous interest and that made ISM physics a major astrophysical research topic, not only in Germany but worldwide. Recently, tremendous progress has been made in identifying the various processes that shape the ISM. It has become clear that its non-linear dynamics and multi-scale structure require ...
Probing nuclear activity versus star formation at z ∼ 0.8 using near
... as the AGN contributes to both the continuum and the emission line spectrum. Thus, estimates of the SFRs of powerful AGN, as for example quasars, will be contaminated with AGN emission to a certain extent. On the other hand, the SFRs of deeply buried and optically dull AGN obtained from Hα emission ...
... as the AGN contributes to both the continuum and the emission line spectrum. Thus, estimates of the SFRs of powerful AGN, as for example quasars, will be contaminated with AGN emission to a certain extent. On the other hand, the SFRs of deeply buried and optically dull AGN obtained from Hα emission ...
Observational evidence for AGN feedback in early
... A major amendment in recent models of hierarchical galaxy formation is the inclusion of socalled active galactic nucleus (AGN) feedback. The energy input from an active central massive black hole is invoked to suppress star formation in early-type galaxies at later epochs. A major problem is that th ...
... A major amendment in recent models of hierarchical galaxy formation is the inclusion of socalled active galactic nucleus (AGN) feedback. The energy input from an active central massive black hole is invoked to suppress star formation in early-type galaxies at later epochs. A major problem is that th ...
A catalogue of the Chandra Deep Field South with multi
... 3.1. Image reduction and object search All procedures used for the data reduction are based on the MIDAS package. A WFI image processing pipeline was developed by Wolf et al. (2001) and makes intensive use of programmes developed by K. Meisenheimer, H.-J. Röser and H. Hippelein for the Calar Alto D ...
... 3.1. Image reduction and object search All procedures used for the data reduction are based on the MIDAS package. A WFI image processing pipeline was developed by Wolf et al. (2001) and makes intensive use of programmes developed by K. Meisenheimer, H.-J. Röser and H. Hippelein for the Calar Alto D ...
Article PDF - IOPscience
... a resolution of R ∼ 600 with wavelength coverage from 9.9 to 37.2 μm; the short-low (SL1 and SL2) and long-low (LL1 and LL2) modules operate at resolutions R ∼ 56–127, with coverage spanning 5.2–38 μm. There also exist two “bonus segments” that cover the overlapping range between the first and secon ...
... a resolution of R ∼ 600 with wavelength coverage from 9.9 to 37.2 μm; the short-low (SL1 and SL2) and long-low (LL1 and LL2) modules operate at resolutions R ∼ 56–127, with coverage spanning 5.2–38 μm. There also exist two “bonus segments” that cover the overlapping range between the first and secon ...
New Worlds, New Horizons in Astronomy and
... scholars engaged in scientific and engineering research, dedicated to the furtherance of science and technology and to their use for the general welfare. Upon the authority of the charter granted to it by the Congress in 1863, the Academy has a mandate that requires it to advise the federal governme ...
... scholars engaged in scientific and engineering research, dedicated to the furtherance of science and technology and to their use for the general welfare. Upon the authority of the charter granted to it by the Congress in 1863, the Academy has a mandate that requires it to advise the federal governme ...
The visibility of Lyman Alpha Emitters: constraining reionization
... radiative transfer code (pCRASH). We post-process the cosmological simulation with pCRASH using five different values of the escape fraction of hydrogen ionizing photons (fesc = 0.05, 0.25, 0.5, 0.75, 0.95) until reionization is complete, i.e. the average neutral hydrogen fraction drops to hχHI i ≃ ...
... radiative transfer code (pCRASH). We post-process the cosmological simulation with pCRASH using five different values of the escape fraction of hydrogen ionizing photons (fesc = 0.05, 0.25, 0.5, 0.75, 0.95) until reionization is complete, i.e. the average neutral hydrogen fraction drops to hχHI i ≃ ...
Annual Report 2006/2007
... halos of unknown constitution. Astronomers are able to look back in time, by observing galaxies at ever greater distances. Because light travels at finite velocity, distant objects are seen at a time when the Universe was young. The expansion of the Universe causes light to be redshifted, so that th ...
... halos of unknown constitution. Astronomers are able to look back in time, by observing galaxies at ever greater distances. Because light travels at finite velocity, distant objects are seen at a time when the Universe was young. The expansion of the Universe causes light to be redshifted, so that th ...
Markov Chain Monte Carlo Modeling of High-Redshift Quasar
... Schmidt (1963) from the optical spectrum of a variable star-like object coincident with the radio source 3C 273. It was found to have a blue non-thermal power-law continuum spectrum Fν ∝ ν 0.28 (Oke 1963), where Fν is the flux density per unit frequency and ν is the frequency. The power-law spectrum ...
... Schmidt (1963) from the optical spectrum of a variable star-like object coincident with the radio source 3C 273. It was found to have a blue non-thermal power-law continuum spectrum Fν ∝ ν 0.28 (Oke 1963), where Fν is the flux density per unit frequency and ν is the frequency. The power-law spectrum ...
Was a cloud-cloud collision the trigger of the recent star formation in
... Given the elongated appearance of the high- and low-velocity clouds in Serpens, we hypothesised that the velocity structure of the Serpens cluster is caused by the collision of two elongated clouds (∼1 pc long). Cloud collisions have long been thought to be an important process in the ISM (since Oor ...
... Given the elongated appearance of the high- and low-velocity clouds in Serpens, we hypothesised that the velocity structure of the Serpens cluster is caused by the collision of two elongated clouds (∼1 pc long). Cloud collisions have long been thought to be an important process in the ISM (since Oor ...
The old globular cluster system of the dIrr galaxy NGC 1427A in the
... using multi-wavelength VLT observations in U, B, V, I, Hα , J, H, and Ks bands under excellent observing conditions. We applied color and size selection criteria to select old GC candidates and made use of archival ACS images taken with the Hubble Space Telescope to reject contaminating background s ...
... using multi-wavelength VLT observations in U, B, V, I, Hα , J, H, and Ks bands under excellent observing conditions. We applied color and size selection criteria to select old GC candidates and made use of archival ACS images taken with the Hubble Space Telescope to reject contaminating background s ...
ALMA - ESO
... Detect the Milky Way at z=3 Measure dust broadband emission and spectral line radiation from atoms and molecules in high-z galaxies to obtain detailed morphology and kinematics ...
... Detect the Milky Way at z=3 Measure dust broadband emission and spectral line radiation from atoms and molecules in high-z galaxies to obtain detailed morphology and kinematics ...
THE STAR FORMATION AND NUCLEAR ACCRETION HISTORIES OF NORMAL GALAXIES
... shallow, however, to detect typical galaxies even at modest redshifts. Fortunately, the wide area of the survey allows us to measure the mean properties of a large, representative population of galaxies by “stacking” (averaging) their X-ray emission (Brandt et al. 2001; Nandra et al. 2002; Hornschem ...
... shallow, however, to detect typical galaxies even at modest redshifts. Fortunately, the wide area of the survey allows us to measure the mean properties of a large, representative population of galaxies by “stacking” (averaging) their X-ray emission (Brandt et al. 2001; Nandra et al. 2002; Hornschem ...
ASI 2017 Abstract Book - Astronomical Society of India
... One of the most outstanding challenges in extragalactic astronomy is to identify the astrophysical processes responsible for transforming simple dark matter haloes into the heterogenous population of galaxies inhabiting today's Universe. How did different morphological types form and evolve? Does th ...
... One of the most outstanding challenges in extragalactic astronomy is to identify the astrophysical processes responsible for transforming simple dark matter haloes into the heterogenous population of galaxies inhabiting today's Universe. How did different morphological types form and evolve? Does th ...
Formation of Molecular Clouds and Global Conditions for Star
... (Evans et al. 2009; Heiderman et al. 2010; Lada et al. 2010, 2012). These relations take on different shapes at different scales. Early studies of whole galaxies found a power-law correlation between total gas content (H I plus H2 ) and star formation rate (SFR) with an index N ∼ 1.5 (Kennicutt 1989 ...
... (Evans et al. 2009; Heiderman et al. 2010; Lada et al. 2010, 2012). These relations take on different shapes at different scales. Early studies of whole galaxies found a power-law correlation between total gas content (H I plus H2 ) and star formation rate (SFR) with an index N ∼ 1.5 (Kennicutt 1989 ...
A Comet-Hunter`s Legacy -
... by each other, they undergo episodes of star formation caused by their gravitational interaction. M81's bright spiral arms are the site of star formation, partially caused by density waves raised by the most recent passage of M82, and the central portion of M82 is undergoing a starburst -- an explos ...
... by each other, they undergo episodes of star formation caused by their gravitational interaction. M81's bright spiral arms are the site of star formation, partially caused by density waves raised by the most recent passage of M82, and the central portion of M82 is undergoing a starburst -- an explos ...
Where stars form: inside-out growth and coherent star formation from
... 2676 galaxies enabling a division into subsamples based on stellar mass and star formation rate. By creating deep stacked Hα images, we reach surface brightness limits of 1 × 10−18 erg s−1 cm−2 arcsec−2 , allowing us to map the distribution of ionized gas out to greater than 10 kpc for typical L∗ ga ...
... 2676 galaxies enabling a division into subsamples based on stellar mass and star formation rate. By creating deep stacked Hα images, we reach surface brightness limits of 1 × 10−18 erg s−1 cm−2 arcsec−2 , allowing us to map the distribution of ionized gas out to greater than 10 kpc for typical L∗ ga ...
LIGO SURF 2006 Lecture 1 - Indico
... Quasar image appears around the central glow formed by nearby galaxy. Such gravitational lensing images are used to detect a ‘dark matter’ body as the central object ...
... Quasar image appears around the central glow formed by nearby galaxy. Such gravitational lensing images are used to detect a ‘dark matter’ body as the central object ...
Astronomy and Astrophysics (ASTRO) Iowa State University – 2013-2014 1
... equations and constitutive relations: energy generation, energy transport by radiation and convection; equation of state, nuclear energy generation and nucleosynthesis. Numerical and analytic solutions to the equations of structure and evolution. Observational connections through the theory of radia ...
... equations and constitutive relations: energy generation, energy transport by radiation and convection; equation of state, nuclear energy generation and nucleosynthesis. Numerical and analytic solutions to the equations of structure and evolution. Observational connections through the theory of radia ...
SPICA Yellow Book
... through the investigation of the cold and obscured parts of the Universe, where the basic processes of formation and evolution occur. Deep exploration of the cold Universe using high spatial resolution observations in the Far Infrared (FIR) and sub-mm started in 2009 with the launch of the Herschel ...
... through the investigation of the cold and obscured parts of the Universe, where the basic processes of formation and evolution occur. Deep exploration of the cold Universe using high spatial resolution observations in the Far Infrared (FIR) and sub-mm started in 2009 with the launch of the Herschel ...