202,708 research outputs found
Tully, P M, NX38135
No full textThis record was harvested from a previous catalogue system and will be withdrawn in 2025. Information in this record may be superseded or incomplete. Visit this record in UMA's new catalogue at: https://archives.library.unimelb.edu.au/nodes/view/422316Surname: TULLY. Given Name(s) or Initials: P M. Military Service Number or Last Known Location: NX38135. Missing, Wounded and Prisoner of War Enquiry Card Index Number: 20781.247799
Item: [2016.0049.54577] "Tully, P M, NX38135
Tully, M, VX4708
No full textThis record was harvested from a previous catalogue system and will be withdrawn in 2025. Information in this record may be superseded or incomplete. Visit this record in UMA's new catalogue at: https://archives.library.unimelb.edu.au/nodes/view/422325Surname: TULLY. Given Name(s) or Initials: M. Military Service Number or Last Known Location: VX4708. Missing, Wounded and Prisoner of War Enquiry Card Index Number: 8843.247817
Item: [2016.0049.54586] "Tully, M, VX4708
ZFIRE : the evolution of the stellar mass Tully-Fisher relation to redshift ∼ 2.2
No full textUsing observations made with MOSFIRE on Keck I as part of the ZFIRE survey, we present the stellar mass Tully-Fisher relation at 2.0 < z < 2.5. The sample was drawn from a stellar-mass-limited, K-s-band-selected catalog from ZFOURGE over the CANDELS area in the COSMOS field. We model the shear of the Ha emission line to derive rotational velocities at 2.2 x the scale radius of an exponential disk (V-2.2). We correct for the blurring effect of a 2D point-spread function (PSF) and the fact that the MOSFIRE PSF is better approximated by a Moffat than a Gaussian, which is more typically assumed for natural seeing. We find for the Tully-Fisher relation at 2.0 < z < 2.5 that log V-2.2=(2.18 +/- 0.051)+(0.193 +/- 0.108)(logM/M-circle dot - 10) and infer an evolution of the zero- point of Delta M/M-circle dot = - 0.25 +/- 0.16 dex or Delta M/M-circle dot = -0.39 +/- 0.21 dex compared to z = 0 when adopting a fixed slope of 0.29 or 1/4.5, respectively. We also derive the alternative kinematic estimator S-0.5, with a best-fit relation log S-0.5=(2.06 +/- 0.032) + (0.211 +/- 0.086) (logM/M-circle dot - 10), and infer an evolution of Delta M/M-circle dot = -0.45 +/- 0.13 dex compared to z < 1.2 if we adopt a fixed slope. We investigate and review various systematics, such as PSF effects, projection effects, systematics related to stellar mass derivation, selection biases, and slope. We find that discrepancies between the various literature values are reduced when taking these into account. Our observations correspond well with the gradual evolution predicted by semianalytic models
The Baryonic Tully-Fisher Relation
No full textWe explore the Tully-Fisher relation over five decades in stellar mass in galaxies with circular velocities ranging over 30 ≲ Vc ≲ 300 km s-1. We find a clear break in the optical Tully-Fisher relation: field galaxies with Vc ≲ 90 km s-1 fall below the relation defined by brighter galaxies. These faint galaxies, however, are very rich in gas; adding in the gas mass and plotting the baryonic disk mass Md = M* + Mgas in place of luminosity restores the single linear relation. The Tully-Fisher relation thus appears fundamentally to be a relation between rotation velocity and total baryonic mass of the form Md ∝ V4c
The hierarchical build-up of the Tully-Fisher relation
No full textWe use the semi-analytic model GalICS to predict the Tully-Fisher relation in the B, I and for the first time, in the K band, and its evolution with redshift, up to z~1. We refined the determination of the disk galaxies rotation velocity, with a dynamical recipe for the rotation curve, rather than a simple conversion from the total mass to maximum velocity. The new recipe takes into account the disk shape factor, and the angular momentum transfer occurring during secular evolution leading to the formation of bulges. This produces model rotation velocities that are lower by ~20-25% for the majority of the spirals. We implemented stellar population models with a complete treatment of the TP-AGB, which leads to a revision of the mass-to-light ratio in the near-IR. I/K band luminosities increase by ~0.3/0.5 mags at redshift z=0 and by ~0.5/1 mags at z=3. With these two new recipes in place, the comparison between the predicted Tully-Fisher relation with a series of datasets in the optical and near-IR, at redshifts between 0 and 1, is used as a diagnostics of the assembly and evolution of spiral galaxies in the model. At 0.
Pre-clearing vegetation of the coastal lowlands of the Wet Tropics Bioregion, North Queensland
No full textA pre-clearing vegetation map and digital coverage at approximately 1:50 000 scale for the coastal lowlands (up to about 200 m elevation) of the Wet Tropics Bioregion, North Queensland is presented. The study area covers about 508 000 ha from Cooktown, 420 km south almost to Townsville (latitude 15° 30’–18° 20’ longitude 144° 50’–146° 40’). Data sources included historical aerial photography, early surveyors’ plans, explorers’ journals, previous vegetation maps, and maps of soils and geology. The pre-clearing mapping was built around the remnant vegetation mapping of Stanton & Stanton (2005), and the vegetation classification of this latter work was adopted. Vegetation units were further classified into regional ecosystems compatible with the standard State-wide system used by Queensland government. The digital coverage is part of the current Queensland Herbarium regional ecosystem coverage (Queensland Herbarium and Wet Tropics Management Authority 2005). Coloured maps (1:100 000 scale) of the pre-clearing vegetation of the Herbert, Tully, Innisfail and Macalister/Daintree subregions are on an accompanying CD-ROM. An evaluation of vegetation loss through clearing on the coastal lowlands of the Wet Tropics revealed several nearextinct vegetation communities and regional ecosystems, and many others that are drastically reduced in area. Even ecosystems occurring on poorly drained lands have suffered a surprisingly high level of loss due to the effectiveness of drainage operations. Grassland ecosystems were found to be widespread on the Herbert and Tully floodplains, but are now close to extinction. The lowlands vegetation of the Wet Tropics that remains today continues to be fragmented and degraded despite the introduction of State-wide broad-scale tree-clearing laws in 1999, and the cessation of broadscale tree-clearing in December 2006
NONLINEARITY OF THE TULLY-FISHER RELATION
No full textA systematic variation of the dark matter abundance in spiral galaxies, previously reported (Persic & Salucci), accounts for the observed non-linearity of the Tully-Fisher relation. Increasing proportions of dark mass at low luminosities, as revealed by optical rotation curves, make faint galaxies shift to higher rotation velocities for a given luminosity, thus inducing a curvature in the velocity-luminosity correlation
The Calibration of the WISE W1 and W2 Tully-Fisher Relation
No full text22 page, 21 figures, accepted to ApJ, Table 1 data at http://spartan.srl.caltech.edu/~neill/tfwisecal/table1.txtIn order to explore local large-scale structures and velocity fields, accurate galaxy distance measures are needed. We now extend the well-tested recipe for calibrating the correlation between galaxy rotation rates and luminosities -- capable of providing such distance measures -- to the all-sky, space-based imaging data from the Wide-field Infrared Survey Explorer (WISE) W1 (m) and W2 (m) filters. We find a linewidth to absolute magnitude correlation (known as the Tully-Fisher Relation, TFR) of (0.54 magnitudes rms) and (0.56 magnitudes rms) from 310 galaxies in 13 clusters. We update the I-band TFR using a sample 9% larger than in Tully & Courtois (2012). We derive (0.46 magnitudes rms). The WISE TFRs show evidence of curvature. Quadratic fits give (0.52 magnitudes rms) and (0.55 magnitudes rms). We apply an I-band -- WISE color correction to lower the scatter and derive and (both 0.46 magnitudes rms). Using our three independent TFRs (W1 curved, W2 curved and I-band), we calibrate the UNION2 supernova Type Ia sample distance scale and derive (stat) (sys) kms Mpc with 4% total error
ON THE TURNOVER OF THE TULLY-FISHER RELATION
No full textThe observed turnover at the high linewidth end of the infrared Tully-Fisher relation can be explained by the stellar population differences among galaxies. When the IRAS 60 mu m fluxes are added to the Tully-Fisher relation as a second parameter, the turnover disappears and the scatter becomes smaller, from 0.35 to 0.25 mag
ON THE TURNOVER OF THE TULLY-FISHER RELATION
No full textThe observed turnover at the high linewidth end of the infrared Tully-Fisher relation can be explained by the stellar population differences among galaxies. When the IRAS 60 mu m fluxes are added to the Tully-Fisher relation as a second parameter, the turnover disappears and the scatter becomes smaller, from 0.35 to 0.25 mag.</p
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