Systematics of bulge-to-disk ratios

Simien, F.; Vaucouleurs, G. de

doi:10.1086/164015

Cited by 368 publications

(398 citation statements)

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“…Following the relation found by Simien & de Vaucouleurs (1986), we used the B/T values to assign our galaxies a specific Hubble class, which is needed to obtain the galaxyspecific SN rate. We use the SNuB values and relations provided by Li et al (2011a) to simulate SNe Ia, SNe Ibc and SNe II.…”

Section: B3 Transient Modelsmentioning

confidence: 99%

Gaiatransient detection efficiency: hunting for nuclear transients

Blagorodnova

Velzen

Harrison

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a study of the detectability of transient events associated with galaxies for the Gaia European Space Agency astrometric mission. We simulated the on-board detections, and on-ground processing for a mock galaxy catalogue to establish the properties required for the discovery of transient events by Gaia, specifically tidal disruption events (TDEs) and supernovae (SNe). Transients may either be discovered by the on-board detection of a new source or by the brightening of a previously known source. We show that Gaia transients can be identified as new detections on-board for offsets from the host galaxy nucleus of 0.1-0.5 arcsec, depending on magnitude and scanning angle. The Gaia detection system shows no significant loss of SNe at close radial distances to the nucleus. We used the detection efficiencies to predict the number of transients events discovered by Gaia. For a limiting magnitude of 19, we expect around 1300 SNe per year: 65% SN Ia, 28% SN II and 7% SN Ibc, and ∼20 TDEs per year.

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Section: B3 Transient Modelsmentioning

confidence: 99%

Gaiatransient detection efficiency: hunting for nuclear transients

Blagorodnova

Velzen

Harrison

et al. 2015

Mon. Not. R. Astron. Soc.

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“…The massive S0 galaxy (hereafter called gS0) is composed of a spherical dark matter halo and a spherical stellar bulge, both of which (Binney & Tremaine 1987) with mass M * , and vertical and radial scale-lengths of h * and a * , respectively ( Table 1). The adopted bulge-to-total baryonic mass ratio of our S0 galaxy model, B/T of 1:5, is based on the most recent estimate for the ratios of S0 galaxies (Laurikainen et al 2007), which are up to a factor 3 lower than earlier estimates (e.g., Simien & de Vaucouleurs 1986). As the work of Laurikainen et al (2007) is based on K s band (2.2 μm) data, it represents more realistic values for the old stellar component than those by Simien & de Vaucouleurs (1986) based on B-band data (the dust extinction being more significant at these wavelengths).…”

Section: Models and Initial Conditionsmentioning

confidence: 99%

The slowing down of galaxy disks in dissipationless minor mergers

Matteo

Lehnert

et al. 2010

A&A

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We have investigated the impact of dissipationless minor galaxy mergers on the angular momentum of the remnant. Our simulations cover a range of initial orbital characteristics, and the system consists of a massive galaxy with a bulge and disk merging with a much less massive (one-tenth or one-twentieth) gasless companion that has a variety of morphologies (disk-or elliptical-like) and central baryonic mass concentrations. During the process of merging, the orbital angular momentum is redistributed into the internal angular momentum of the final system; the internal angular momentum of the primary galaxy can increase or decrease depending on the relative orientation of the orbital spin vectors (direct or retrograde), while the initially nonrotating dark matter halo always gains angular momentum. The specific angular momentum of the stellar component always decreases independently of the orbital parameters or morphology of the satellite, the decrease in the rotation velocity of the primary galaxy is accompanied by a change in the anisotropy of the orbits, and the ratio of rotation speed to velocity dispersion of the merger remnant is lower than the initial value, not only because of an increase in the dispersion but also of the slowing-down of the disk rotation. We briefly discuss several astrophysical implications of these results, suggesting that minor mergers do not cause a "random walk" process of the angular momentum of the stellar disk component of galaxies, but rather a steady decrease. Minor mergers may play a role in producing the large scatter observed in the Tully-Fisher relation for S0 galaxies, as well as in the increase of the velocity dispersion and the decrease in v/σ at large radii as observed in S0 galaxies.

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“…Galaxy morphology in the model is determined by the ratio of the B-band luminosities of the disk and bulge components which correlates well with Hubble type (Simien & de Vaucouleurs 1986). A morphology index is defined as…”

Section: The Modelmentioning

confidence: 99%

Identifying the progenitor set of present-day early-type galaxies: a view from the standard model

Kaviraj

Devriendt

Ferreras³

et al. 2009

A&A

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We present a comprehensive theoretical study, using a semi-analytical model within the standard LCDM framework, of the photometric properties of the progenitors of present-day early-type galaxies in the redshift range 0 < z < 1. We explore progenitors of all morphologies and study their characteristics as a function of the luminosity and local environment of the early-type remnant at z = 0. In agreement with previous studies, we find that, while larger early-types are generally assembled later, their luminosity-weighted stellar ages are typically older. In dense cluster-like environments, ∼70 percent of early-type systems are "in place" by z = 1 and evolve without interactions thereafter, while in the field the corresponding value is ∼30 percent. Averaging across all environments at z ∼ 1, less than 50 percent of the stellar mass which ends up in early-types today is actually in early-type progenitors at this redshift, in agreement with recent observational work. The corresponding value is ∼65 percent in clusters, due to faster morphological evolution in such dense environments. We develop probabilistic prescriptions which provide a means of including spiral (i.e. non early-type) progenitors at intermediate and high redshifts, based on their luminosity and optical colours. For example, we find that, at intermediate redshifts (z ∼ 0.5), large (M V < −21.5), red (B − V > 0.7) spirals have ∼75-95 percent chance of being an early-type progenitor, while the corresponding probability for large blue spirals (M B < −21.5, B − V < 0.7) is ∼50-75 percent. The prescriptions developed here can be used to address, from the perspective of the standard model, the issue of "progenitor bias", whereby the exclusion of late-type progenitors in observational studies can lead to inaccurate conclusions regarding the evolution of the early-type population over cosmic time. Finally, we explore the correspondence between the true "progenitor set" of the present-day early-type population -defined as the set of all galaxies that are progenitors of present-day early-types regardless of their morphologies -and the frequently used "red-sequence", defined as the set of galaxies within the part of the colour-magnitude space which is dominated by early-type objects. We find that, while more massive members (M V ≤ −21) of the "red sequence" trace the progenitor set reasonably well, the relationship breaks down at fainter luminosities (M V ≥ −21). Thus, while the results of recent observational studies which exploit the red sequence are valid (since they are largely restricted to massive galaxies), more care should be taken when deeper observations (which will probe fainter luminosities) become available in the future.

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Systematics of bulge-to-disk ratios

Cited by 368 publications

References 0 publications

Gaiatransient detection efficiency: hunting for nuclear transients

Gaiatransient detection efficiency: hunting for nuclear transients

The slowing down of galaxy disks in dissipationless minor mergers

Identifying the progenitor set of present-day early-type galaxies: a view from the standard model

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