The Physical Origins of The Morphology
... and Padilla & Strauss (2008). Such an approach is complementary to studies of morphology, defined either visually or otherwise, because it makes no assumptions about the connection with galaxy structure. Because, in addition, we select our sample spectroscopically, our analysis is completely indepen ...
... and Padilla & Strauss (2008). Such an approach is complementary to studies of morphology, defined either visually or otherwise, because it makes no assumptions about the connection with galaxy structure. Because, in addition, we select our sample spectroscopically, our analysis is completely indepen ...
Galaxy Formation and Evolution.
... H O U J U N M O is Professor of Astrophysics at the University of Massachusetts. He is known for his work on the formation and clustering of galaxies and their dark matter halos. F R A N K VA N D E N B O S C H is Assistant Professor at Yale University, and is known for his studies of the formation, ...
... H O U J U N M O is Professor of Astrophysics at the University of Massachusetts. He is known for his work on the formation and clustering of galaxies and their dark matter halos. F R A N K VA N D E N B O S C H is Assistant Professor at Yale University, and is known for his studies of the formation, ...
β Relation for Local Galaxies
... galaxies on the IRX show a considerable amount of scatter compared to the starburst IRX relation. Currently, no single relation for normal star-forming galaxies exists between βGLX the UV attenuation nor is there agreement as to the underlying physical reason that causes the spread. It is necessary ...
... galaxies on the IRX show a considerable amount of scatter compared to the starburst IRX relation. Currently, no single relation for normal star-forming galaxies exists between βGLX the UV attenuation nor is there agreement as to the underlying physical reason that causes the spread. It is necessary ...
Galaxy morphology, luminosity, and environment in the SDSS DR7
... most accurate, but by far the most time consuming approach is to use visual classification (Marzke et al. 1994, 1998; Kochanek et al. 2001; Cuesta-Bolao & Serna 2003; Nakamura et al. 2003). For the SDSS survey, visual classification has become possible thanks to the Galaxy Zoo project (Lintott et al ...
... most accurate, but by far the most time consuming approach is to use visual classification (Marzke et al. 1994, 1998; Kochanek et al. 2001; Cuesta-Bolao & Serna 2003; Nakamura et al. 2003). For the SDSS survey, visual classification has become possible thanks to the Galaxy Zoo project (Lintott et al ...
The KMOS Redshift One Spectroscopic Survey
... high redshift galaxies with much greater efficiency. KMOS allows for simultaneous observations with up to 24 IFUs within a 7.2 arcminute diameter radius and is thus perfectly suited to such a task. The KMOS Redshift One Spectroscopic Survey (KROSS) is a European Southern Observatory (ESO) guaranteed ...
... high redshift galaxies with much greater efficiency. KMOS allows for simultaneous observations with up to 24 IFUs within a 7.2 arcminute diameter radius and is thus perfectly suited to such a task. The KMOS Redshift One Spectroscopic Survey (KROSS) is a European Southern Observatory (ESO) guaranteed ...
http://arxiv.org/pdf/1401.1510v1.pdf
... most luminous QSOs, i.e those likely associated with the formation of massive quiescent galaxies, are found to be primarily major mergers (Treister et al. 2012; Riechers et al. 2008), a result which is cooborated by Olsen et al. (2013) who find that luminous AGN in massive z ∼ 2 galaxies must be tri ...
... most luminous QSOs, i.e those likely associated with the formation of massive quiescent galaxies, are found to be primarily major mergers (Treister et al. 2012; Riechers et al. 2008), a result which is cooborated by Olsen et al. (2013) who find that luminous AGN in massive z ∼ 2 galaxies must be tri ...
Dust attenuation up to z ≃ 2 in the AKARI North Ecliptic Pole Deep
... Methods. We selected galaxies in the mid-IR from the deep survey of the North Ecliptic Field performed by the AKARI satellite. Using multiple filters of IRC instrument, we selected more than 4000 galaxies from their rest-frame emission at 8 µm, from z ' 0.2 to ∼2. We built spectral energy distributi ...
... Methods. We selected galaxies in the mid-IR from the deep survey of the North Ecliptic Field performed by the AKARI satellite. Using multiple filters of IRC instrument, we selected more than 4000 galaxies from their rest-frame emission at 8 µm, from z ' 0.2 to ∼2. We built spectral energy distributi ...
Catalogues of isolated galaxies, isolated pairs, and isolated triplets
... been hampered by scarce redshift information. The new 3-dimensional (3D) surveys permit small, faint, physically bound satellites to be distinguished from a background-projected galaxy population, giving a more comprehensive 3D picture of the surroundings. Aims. We aim to provide representative samp ...
... been hampered by scarce redshift information. The new 3-dimensional (3D) surveys permit small, faint, physically bound satellites to be distinguished from a background-projected galaxy population, giving a more comprehensive 3D picture of the surroundings. Aims. We aim to provide representative samp ...
The impact of protocluster environments at z = 1.6
... around Cl 0218.3−0510 using photometric redshifts. The centre of the field of view lies at 02h 18m 28.s 75, −05d 09m 52.s 19. Full details of the data and methods used to select the protocluster galaxies are provided in Hatch et al. (2016) which we summarize here. A K-selected UBVRi z JHK[3.6][4.5 ...
... around Cl 0218.3−0510 using photometric redshifts. The centre of the field of view lies at 02h 18m 28.s 75, −05d 09m 52.s 19. Full details of the data and methods used to select the protocluster galaxies are provided in Hatch et al. (2016) which we summarize here. A K-selected UBVRi z JHK[3.6][4.5 ...
The Evolution of the Mass-Size relation to z = 3.5 in the GOODS
... field, we also study sizes of the Sub-millimetre galaxies (SMGs) as a population of star forming galaxies at high redshifts. The subsample of SMGs for our studies is drawn from Chapman et al. (2005) and Pope et al. (2006). The catalog of SMGs provided by Pope et al. (2006) contains 35 candidates fro ...
... field, we also study sizes of the Sub-millimetre galaxies (SMGs) as a population of star forming galaxies at high redshifts. The subsample of SMGs for our studies is drawn from Chapman et al. (2005) and Pope et al. (2006). The catalog of SMGs provided by Pope et al. (2006) contains 35 candidates fro ...
astro-ph/9704019 2 Apr 1997 - National Optical Astronomy
... primarily as a necessary ‘correction’ to apply in the grander quest for the nature of the world model; the term ‘evolutionary correction’ remains (c.f. Poggianti 1997). Galaxy evolution only rose to prominence when quantitative predictions for the star formation histories of normal galaxies became a ...
... primarily as a necessary ‘correction’ to apply in the grander quest for the nature of the world model; the term ‘evolutionary correction’ remains (c.f. Poggianti 1997). Galaxy evolution only rose to prominence when quantitative predictions for the star formation histories of normal galaxies became a ...
Euclid - at www.arxiv.org.
... Understanding the acceleration of the expansion of the Universe is one of the most compelling challenges of cosmology and fundamental physics. The Euclid surveys will show how cosmic acceleration modifies the expansion history and the 3-dimensional distribution of matter in the Universe. To achieve ...
... Understanding the acceleration of the expansion of the Universe is one of the most compelling challenges of cosmology and fundamental physics. The Euclid surveys will show how cosmic acceleration modifies the expansion history and the 3-dimensional distribution of matter in the Universe. To achieve ...
IDEA MAN
... interstellar gas could produce cosmic rays outside the supernova itself. Second, Baade and Zwicky tried to explain how such titanic explosions could occur at all. Then as now, any reasonable theory had to involve gravitational collapse. However, a simple calculation showed that the collapsing progen ...
... interstellar gas could produce cosmic rays outside the supernova itself. Second, Baade and Zwicky tried to explain how such titanic explosions could occur at all. Then as now, any reasonable theory had to involve gravitational collapse. However, a simple calculation showed that the collapsing progen ...
A Wide-Field Study of the z~ 0.8 Cluster RX J0152. 7
... of the cluster mass function indicate that the number of massive clusters increases by a factor of a few since such redshifts (Vikhlinin et al. 2008). In addition, as noted above, simulations suggest that individual clusters grow in mass by a factor of ∼ 2 − 3 over the same time period (Wechsler et ...
... of the cluster mass function indicate that the number of massive clusters increases by a factor of a few since such redshifts (Vikhlinin et al. 2008). In addition, as noted above, simulations suggest that individual clusters grow in mass by a factor of ∼ 2 − 3 over the same time period (Wechsler et ...
- Max-Planck-Institut für Astronomie
... which timescale these selection criteria are sensitive, we explore the characteristics of a suite of N-body simulation mergers between spheroid-dominated galaxies (x 3.1). We then apply these selection criteria to the data in x 3.2. We use these results to derive a dry merger fraction and incidence ...
... which timescale these selection criteria are sensitive, we explore the characteristics of a suite of N-body simulation mergers between spheroid-dominated galaxies (x 3.1). We then apply these selection criteria to the data in x 3.2. We use these results to derive a dry merger fraction and incidence ...
HI in Early-type Galaxies
... morphology, indicating that the gas is accreting onto the galaxy, or is left over from a recent merger event. A good example of this is NGC 5266 (Figure 4; see Morganti et al. 1997a). This is a minor-axis dust-lane elliptical with a large amount of HI (∼1010 M¯ , MHI /LB ∼ 0 · 2). Almost all the HI ...
... morphology, indicating that the gas is accreting onto the galaxy, or is left over from a recent merger event. A good example of this is NGC 5266 (Figure 4; see Morganti et al. 1997a). This is a minor-axis dust-lane elliptical with a large amount of HI (∼1010 M¯ , MHI /LB ∼ 0 · 2). Almost all the HI ...
MASSIVE GALAXIES IN COSMOLOGICAL SIMULATIONS: ULTRAVIOLET-SELECTED
... We study the properties of galaxies at redshift z ¼ 2 in a cold dark matter (CDM) universe, using two different types of hydrodynamic simulation methods—Eulerian total variation diminishing (TVD) and smoothed particle hydrodynamics (SPH)—and a spectrophotometric analysis in the Un , G, R filter s ...
... We study the properties of galaxies at redshift z ¼ 2 in a cold dark matter (CDM) universe, using two different types of hydrodynamic simulation methods—Eulerian total variation diminishing (TVD) and smoothed particle hydrodynamics (SPH)—and a spectrophotometric analysis in the Un , G, R filter s ...
Head–tail Galaxies: beacons of high
... by the passage of the galaxy through the cluster (Odea & Owen 1985) while WATs are more likely to be associated with dominant cluster galaxies (Owen & Rudnick 1976). Although the distinction between ram pressure and ICM effects, such as ‘cluster weather’ (Burns 1998), is often drawn in literature, w ...
... by the passage of the galaxy through the cluster (Odea & Owen 1985) while WATs are more likely to be associated with dominant cluster galaxies (Owen & Rudnick 1976). Although the distinction between ram pressure and ICM effects, such as ‘cluster weather’ (Burns 1998), is often drawn in literature, w ...
THE RED-SEQUENCE LUMINOSITY FUNCTION IN GALAXY
... more massive galaxies being most actively star forming in the past and the bulk of the star formation activity moving toward less massive galaxies as the universe ages. Although this seems intuitively at odds with hierarchical models, scenarios have been proposed in which star formation progresses i ...
... more massive galaxies being most actively star forming in the past and the bulk of the star formation activity moving toward less massive galaxies as the universe ages. Although this seems intuitively at odds with hierarchical models, scenarios have been proposed in which star formation progresses i ...
AN INTENSIVE HUBBLE SPACE TELESCOPE
... Adaptive Light Curve Template for Type Ia Supernovae (SALT) analysis of SNLS and the value of RB measured in our own galaxy) changes w by 0.04 when considering the typical range of color with redshift found in supernova data sets (Kowalski et al. 2008; Wood-Vasey et al. 2007). The systematic uncerta ...
... Adaptive Light Curve Template for Type Ia Supernovae (SALT) analysis of SNLS and the value of RB measured in our own galaxy) changes w by 0.04 when considering the typical range of color with redshift found in supernova data sets (Kowalski et al. 2008; Wood-Vasey et al. 2007). The systematic uncerta ...
Properties of simulated Milky Way-mass galaxies in loose group and
... automatically refines according to the local particle density in addition to a static refinement of nested regions that reduces the run-time while maintaining high resolution around the galaxy of interest. Details of the refinement scheme are described by Teyssier (2002). ramses includes density- an ...
... automatically refines according to the local particle density in addition to a static refinement of nested regions that reduces the run-time while maintaining high resolution around the galaxy of interest. Details of the refinement scheme are described by Teyssier (2002). ramses includes density- an ...
The dark matter crisis: falsification of the current standard model of
... constraints. The nature of spiral nebulae and the dimensions of the universe were debated in 1920 by Harlow Shaply and Heber Curtis in The Great Debate, but galactic and extragalactic distance scales were proven later (Opik 1922; Hubble 1929). The other “Hypothesis 0ii”, so fundamental that it is us ...
... constraints. The nature of spiral nebulae and the dimensions of the universe were debated in 1920 by Harlow Shaply and Heber Curtis in The Great Debate, but galactic and extragalactic distance scales were proven later (Opik 1922; Hubble 1929). The other “Hypothesis 0ii”, so fundamental that it is us ...
FIELD GALAXIES AND THEIR AGNs: NATURE VERSUS
... The critical mass ∼ 2 × 1010 M¯ in simulations (the cold mode dominates below this mass and the hot mode dominates above it) is close to the observed characteristic mass for a shift in galaxy properties, Mgal ∼ 3 × 1010 M¯ (Kauffmann et al. 2004, Kannappan 2004). Galaxies below the critical mass of ...
... The critical mass ∼ 2 × 1010 M¯ in simulations (the cold mode dominates below this mass and the hot mode dominates above it) is close to the observed characteristic mass for a shift in galaxy properties, Mgal ∼ 3 × 1010 M¯ (Kauffmann et al. 2004, Kannappan 2004). Galaxies below the critical mass of ...
Giant Low Surface Brightness Galaxies
... The really large LSB galaxies are usually referred to as Giant LSB (GLSB) galaxies and are generally isolated systems (Bothun et al. 1993). They are found to lie closer to the walls of voids (Rosenbaum et al. 2009). This review will focus only on GLSB galaxies; their nuclear and disk properties are ...
... The really large LSB galaxies are usually referred to as Giant LSB (GLSB) galaxies and are generally isolated systems (Bothun et al. 1993). They are found to lie closer to the walls of voids (Rosenbaum et al. 2009). This review will focus only on GLSB galaxies; their nuclear and disk properties are ...
Big Bang
The Big Bang theory is the prevailing cosmological model for the universe from the earliest known periods through its subsequent large-scale evolution. The model accounts for the fact that the universe expanded from a very high density and high temperature state, and offers a comprehensive explanation for a broad range of observed phenomena, including the abundance of light elements, the cosmic microwave background, large scale structure, and Hubble's Law. If the known laws of physics are extrapolated beyond where they are valid, there is a singularity. Modern measurements place this moment at approximately 13.8 billion years ago, which is thus considered the age of the universe. After the initial expansion, the universe cooled sufficiently to allow the formation of subatomic particles, and later simple atoms. Giant clouds of these primordial elements later coalesced through gravity to form stars and galaxies.Since Georges Lemaître first noted, in 1927, that an expanding universe might be traced back in time to an originating single point, scientists have built on his idea of cosmic expansion. While the scientific community was once divided between supporters of two different expanding universe theories, the Big Bang and the Steady State theory, accumulated empirical evidence provides strong support for the former. In 1929, from analysis of galactic redshifts, Edwin Hubble concluded that galaxies are drifting apart, important observational evidence consistent with the hypothesis of an expanding universe. In 1965, the cosmic microwave background radiation was discovered, which was crucial evidence in favor of the Big Bang model, since that theory predicted the existence of background radiation throughout the universe before it was discovered. More recently, measurements of the redshifts of supernovae indicate that the expansion of the universe is accelerating, an observation attributed to dark energy's existence. The known physical laws of nature can be used to calculate the characteristics of the universe in detail back in time to an initial state of extreme density and temperature.