共查询到20条相似文献，搜索用时 46 毫秒
1.
We report a catalog of 168 galaxy triplets with line-of-sight velocities V LG < 3500 km/s identified using a percolation criterion, which takes individual properties of galaxies into account. The catalog contains the line-of-sight velocities, K-band magnitudes, and morphological types of galaxies. Our sample of galaxy triplets is characterized by the median values of the line-of-sight velocity dispersion, projected harmonic radius, and crossing time of 40 km/s, 155 kpc, and 3 Gyr, respectively. The median projectedmass and K-band luminosity of our triplets are equal to 5 × 1011 M ⊙ and 15M ⊙/L ⊙, respectively, with the uncertainty of these parameters due mostly to the errors of radial-velocity measurements. The basic properties of triple systems in the Local Supercluster are compared to those of more distant isolated triplets from the KTG and KTS samples. The fraction of triplet members among all galaxies is found be more than 5%. 相似文献
2.
We discuss the problems connected with the measurements and evaluation of line-of-sight velocities, obtained with a scanning photoelectric magnetograph using a line-shifter with enhanced sensitivity. We bring arguments for the validity of the results of our photoelectric Doppler velocity recordings. We have found a network of cellularly shaped patterns in the distribution of photo-electrically measured line-of-sight motions, upflowing in the magnetically quiet (blue-shifted) and downflowing in magnetically active (red-shifted) areas of the photosphere, if the mean velocity level is estimated for a sufficiently large measured area. The features of both directions are mutually complementary. We demonstrate the effect of the shift of the reference zero velocity level on the topology of the line-of-sight velocity maps, and the dependence of this level on the size of the area from which it is estimated. 相似文献
3.
《New Astronomy》2019
We exploit information, including velocities from the fifth data release of the RAdial Velocity Experiment (RAVE), to find evidence of the Lin–Shu type tightly wound spiral density waves in the nearby Galactic disk. The Kunder et al. (2017) catalogue of 471117 stars with derived spectrophotometric distances and line-of-sight velocities are explored to find the geometry and parameters of the velocity field in the extended solar neighborhood. Possible existence of noncircular systematic motions of selected 37,354 disk objects within 2 kpc from the Sun and 500 pc from the Galactic mid-plane together with the ordinary differential rotation are assumed. Both the pitch angle of spiral arms and the spatial location of the Sun within the density–wave pattern and the deviations of the motion of objects from the circular motion are calculated by fitting the stellar line-of-sight velocities in RAVE DR5 with the simplest linear perturbation density–wave model. Two radial wavelengths of the wave pattern of about 0.5 kpc and 1.5 kpc in the solar vicinity are found. We argue that the spiral structure of the Galaxy has an oscillating nature corresponding to a concept of the fairly unstable, low amplitude, tightly wound, and rigidly rotating density waves. 相似文献
4.
T. G. Sitnik 《Astronomy Letters》2003,29(5):311-320
We compare the line-of-sight velocities of stars in OB associations within 3 kpc of the Sun and the molecular clouds closest to them. The Perseus arm is used as an example to show that the line-of-sight velocity ranges in which OB-association stars, molecular clouds, and H II regions ionized by these association stars are observed overlap. The streaming motions produced by density waves in the (l, VLSR) plane were found to lead to an inversion of the distances to objects of the Perseus arm and the interarm space beyond this arm. 相似文献
5.
Maartje Sevenster Prasenjit Saha David Valls-Gabaud Roger Fux 《Monthly notices of the Royal Astronomical Society》1999,307(3):584-594
We determine the most likely values of the free parameters of an N -body model for the Galaxy developed by Fux via a discrete–discrete comparison with the positions on the sky and line-of-sight velocities of an unbiased, homogeneous sample of OH/IR stars. Via Monte Carlo simulation, we find the plausibility of the best-fitting models, as well as the errors on the determined values. The parameters that are constrained best by these projected data are the total mass of the model and the viewing angle of the central bar, although the distribution of the latter has multiple maxima. The other two free parameters, the size of the bar and the (azimuthal) velocity of the Sun, are less well-constrained. The best model has a viewing angle of ∼ 44°, a semimajor axis of 2.5 kpc (corotation radius 4.5 kpc, pattern speed 46 km s−1 kpc−1 ), a bar mass of 1.7×1010 M⊙ and a tangential velocity of the local standard of rest of 171 km s−1 . We argue that the lower values that are commonly found from stellar data for the viewing angle (∼25°) arise when too few coordinates are available, when the longitude range is too narrow or when low latitudes are excluded from the fit. The new constraints on the viewing angle of the Galactic bar from stellar line-of-sight velocities decrease further the ability of the distribution of the bar to account for the observed microlensing optical depth toward Baade's window: our model reproduces only half the observed value. The signal of triaxiality diminishes quickly with increasing latitude, fading within approximately 1 scaleheight (≲3°). This suggests that Baade's window is not a very appropriate region in which to sample bar properties. 相似文献
6.
By studying time variations in line-of-sight velocity in prominences, we found that the velocity oscillations with periods over 40 min have a reasonably well-marked dependence of the period length on the heliolatitude. Simultaneous observations of line-of-sight velocities in the photosphere and chromosphere showed that quasi-hourly oscillation periods at these levels of the solar atmosphere and in prominences have a similar latitudinal behaviour. Thus, the photosphere, chromosphere and prominences should be regarded as a unified oscillatory system. 相似文献
7.
Spectroscopic observations of twelve M51-type binary galaxies with the 6-m Special Astrophysical Observatory telescope are presented. We constructed the rotation curves for the primary galaxies of each binary system and determined the line-of-sight velocities of their companions from the Hα and [N II] 6583 Å emission lines. 相似文献
8.
We report a catalog of 509 pairs identified among 10403 nearby galaxies with line-of-sight velocities V LG < 3500 km/s. We selected binary systems in accordance with two criteria (“bounding” and “temporal”), which require the physical pair of galaxies to have negative total energy and its components to be located inside the zero-velocity surface. We assume that individual galaxy masses are proportional to their total K-band luminosities, M = L K × 6M ⊙/L ⊙. The catalog gives the magnitudes and morphological types of galaxies and also the projected (orbital) masses and pair isolation indices. The component line-of-sight velocity differences and projected distances of the binary systems considered have power-law distributions with the median values of 35 km/s and 123 kpc, respectively. The median mass-to-K-band luminosity ratio is equal to 11M ⊙/L ⊙, and its uncertainty is mostly due to the errors of measured velocities. Our sample of binary systems has a typical density contrast of δρ/ρ c ～ 500 and a median crossing time of about 3.5 Gyr. We point out the substantial fraction of binary systems consisting of late-type dwarf galaxies, where the luminosities of both components are lower than that of the Small Magellanic Cloud. The median projected distance for 41 such pairs is only 30 kpc, and the median difference of their line-ofsight velocities is equal to 14 km/s which is smaller than the typical error for radial-velocity (30 km/s). This specific population of gas-rich dwarf binary galaxies such as I Zw 18 may be at the stage immediately before merging of its components. Such objects, which are usually lost in flux-limited (and not distance-limited) samples deserve a thorough study in the HI radio line with high spatial and velocity resolution. 相似文献
9.
Álvaro Villalobos Amina Helmi 《Monthly notices of the Royal Astronomical Society》2009,399(1):166-176
We analyse the phase-space structure of simulated thick discs that are the result of a 5:1 mass-ratio merger between a disc galaxy and a satellite. Our main goal is to establish what would be the imprints of a merger origin for the Galactic thick disc. We find that the spatial distribution predicted for thick-disc stars is asymmetric, seemingly in agreement with recent observations of the Milky Way thick disc. Near the Sun, the accreted stars are expected to rotate more slowly, to have broad velocity distributions and to occupy preferentially the wings of the line-of-sight velocity distributions. The majority of the stars in our model thick discs have low eccentricity orbits (in clear reference to the pre-existing heated disc) which give rise to a characteristic (sinusoidal) pattern for their line-of-sight velocities as a function of galactic longitude. The z -component of the angular momentum of thick-disc stars provides a clear discriminant between stars from the pre-existing disc and those from the satellite, particularly at large radii. These results are robust against the particular choices of initial conditions made in our simulations. 相似文献
10.
J. B. Zirker 《Solar physics》1967,1(2):204-215
Motions in an old center of activity have been studied at the limb with the use of timeresolved H spectra. The observations were made at intervals of 5 seconds over a period of 3/4 hour of good seeing at Sacramento Peak Observatory.Objects in this region have larger line-of-sight velocities than have been reported for spicules in quiet regions. Velocities as high as 70 km/sec were observed; seventeen percent of a sample of 200 instantaneous velocities exceed 30 km/sec.The line-of-sight velocities of 20 objects were measured as a function of time. For 5 of these, transverse velocity components could also be estimated. A single pattern, such as the simple rise without fall reported by Mouradian, does not exist. The motion is often quite complex, involving lateral expansion, shear and occasionally splitting. Reversal of sign of the velocity is not uncommon. 相似文献
11.
Michael R. Merrifield & Konrad Kuijken 《Monthly notices of the Royal Astronomical Society》1998,297(4):1292-1296
We show that the kinematics of the shells seen around some elliptical galaxies provide a new, independent means for measuring the gravitational potentials of elliptical galaxies out to large radii. A numerical simulation of a set of shells formed in the merger between an elliptical and a smaller galaxy reveals that the shells have a characteristic observable kinematic structure, with the maximum line-of-sight velocity increasing linearly as one moves inward from a shell edge. A simple analytic calculation shows that this structure provides a direct measure of the gradient of the gravitational potential at the shell radius. In order to extract this information from attainable data, we have also derived a complete distribution of line-of-sight velocities for material within a shell; comparing the observed spectra of a shell to a stellar template convolved with this distribution will enable us to measure the gradient of the potential at this radius. Repeating the analysis for a whole series of nested shells in a galaxy allows the complete form of the gravitational potential as a function of radius to be mapped out. The requisite observations lie within reach of the up-coming generation of large telescopes. 相似文献
12.
The observed green coronal emission line profiles have been often found to have multi-components. Further examinations reveal that the occurrence of multi-components in line profiles is related to the solar cycle variations as well as the activity of the coronal region. The spatial correspondence between the intense loops in active regions and strong multi-components in line profiles suggests that the presence of loops affects the line shapes. The emission line profiles have been found to be fitted well with single or multi-Gaussians with line-of-sight velocities up to 70 km s–1. A simple radiative transfer model of coronal emission line profiles is developed which shows that coronal loops with mass motions inside may give rise to multi-components in line profiles. The effects of loop parameters such as electron density, flow velocity and kinetic temperature and the line-of-sight variations are studied. It is found that line profiles strongly reflect the physical conditions inside the loop. 相似文献
13.
A new type of oscillations, being long-period oscillations of line-of-sight velocities, with periods ranging from 42 to 82 min and amplitudes in excess of 200 m s-1 has been discovered in prominences. These oscillations may be interpreted as a combination of torsional and longitudinal ones. 相似文献
14.
We demonstrate that the azimuthal ambiguity that is present in solar vector magnetogram data can be resolved with line-of-sight
and horizontal heliographic derivative information by using the divergence-free property of magnetic fields without additional
assumptions. We discuss the specific derivative information that is sufficient to resolve the ambiguity away from disk centre,
with particular emphasis on the line-of-sight derivative of the various components of the magnetic field. Conversely, we also
show cases where ambiguity resolution fails because sufficient line-of-sight derivative information is not available. For
example, knowledge of only the line-of-sight derivative of the line-of-sight component of the field is not sufficient to resolve the ambiguity away from disk centre. 相似文献
15.
Brynildsen N. Brekke P. Fredvik T. Haugan S. V. H. Kjeldseth-Moe O. Maltby P. Harrison R. A. Pike C. D. Rimmele T. Thompson W. T. Wilhelm K. 《Solar physics》1998,179(2):279-312
We have studied the dynamics in the sunspot transition region between the chromosphere and the corona and investigated the extension of the flow field into the corona. Based on EUV spectra of a medium size sunspot and its surroundings, NOAA 7981, observed with CDS and SUMER on SOHO, we derive line-of-sight velocities and study the line profiles for a series of emission lines.The flow field in the low corona is found to differ markedly from that in the transition region. In the transition region the relative line-of-sight velocity shows an upflow in the umbra and relatively large areas with downflow that cover part of the penumbra. The spatial extent of these areas with upflow and downflow increases with increasing temperature in the transition region, but the whole flow field changes character as the temperature increases from the upper transition region to the low corona. Based on a calibration of the SUMER wavelength scale we find that the entire sunspot transition zone appears to be moving downwards towards the chromosphere. The relation between this finding and the general tendency for transition-region lines to show a net red shift is discussed.Several of the transition-region spectral line profiles are observed to show two line components with Gaussian shape and line-of-sight velocities that differ markedly. Several of the line profiles that are composed of two spectral line components occur close to the dividing line between up- and downflow. A discussion of this observation is presented. In small regions with spatial extent of a few arc sec we detect enhanced continuum emission underlying explosive events. The similarities between explosive events with continuum emission and the moustaches observed in H close to sunspots are so striking that we are tempted to introduce the notation transition-region moustaches. 相似文献
16.
Measurements of line-of-sight velocities of quiescent and sunspot prominences on the limb made during the years 1966 and 1968 at Swedish Astrophysical Station in Anacapri, Italy are discussed. Several statistical properties of the velocity field, in particular its connection with close McMath plages are investigated. Results are interpreted in terms of oscillatory motion in prominences. 相似文献
17.
We present profiles of the line-of-sight (l.o.s.) ionospheric wind velocities in the southern auroral/polar region of Saturn. Our velocities are derived from the measurement of Doppler shifting of the H3+ν2Q(1,0−) line at 3.953 microns. The data for this study were obtained using the facility high-resolution spectrometer CSHELL on the NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii, during the night of February 6, 2003 (UT). The l.o.s. velocity profiles finally derived are consistent with an extended region of the upper atmosphere sub-corotating with the planet: the ion velocities in the inertial reference are only 1/3 of those expected for full planetary corotation. We discuss the results in the light of recent proposals for the kronian magnetosphere, and suggest that, in this region, Saturn's ion winds may be under solar wind control. 相似文献
18.
The line-of-sight direction in the redshifted 21-cm signal coming from the cosmic dawn and the epoch of reionization is quite unique in many ways compared to any other cosmological signal. Different unique effects, such as the evolution history of the signal, non-linear peculiar velocities of the matter etc. will imprint their signature along the line-of-sight axis of the observed signal. One of the major goals of the future SKA-LOW radio interferometer is to observe the cosmic dawn and the epoch of reionization through this 21-cm signal. It is thus important to understand how these various effects affect the signal for its actual detection and proper interpretation. For more than one and half decades, various groups in India have been actively trying to understand and quantify the different line-of-sight effects that are present in this signal through analytical models and simulations. In many ways the importance of this sub-field under 21-cm cosmology have been identified, highlighted and pushed forward by the Indian community. In this article, we briefly describe their contribution and implication of these effects in the context of the future surveys of the cosmic dawn and the epoch of reionization that will be conducted by the SKA-LOW. 相似文献
19.
Oscillations of the line-of-sight velocities with periods 82m.2 and 76m.7 were detected in quiescent prominences, with coordinates ? = -75° W and ?= -18° W, respectively. 相似文献
20.
An observational program at the Sacramento Peak Observatory in 1965 provided high-dispersion spectra of the solar chromosphere in several spectral regions simultaneously. These regions included various combinations of the spectral lines Hα, Hβ and H?, the D3-line of Hei, the infrared triplet of Oi, and the H- and K-lines and the infrared triplet of Caii. With the use of an image slicer the observations were made simultaneously at two heights in the solar chromosphere separated by several thousand kilometers. From these data we draw the following conclusions:
- Emission of different lines arises in the same chromospheric features. The intensity ratio of lines of different elements varies significantly from spicule to spicule. For the H- and K-lines of ionized calcium, this ratio remains constant, independent of wavelength throughout the line, overall intensity, and height in the chromosphere. Two rare-earth lines in the wing of the H-line show no spicular structure at all.
- The line-of-sight velocities of many features reverse as a function of time, although most spicules show velocities in only one direction. The simultaneous spectra at two heights show most spicules to have the same line-of-sight velocity at both. There may be an additional class of features, mostly rapidly moving, whose members have line-of-sight velocities that increase with height. These features comprise perhaps 10% of the total. Velocity changes occur simultaneously, to within 20 sec, at two heights separated by 1800 km, indicating velocities of propagation of hundreds of km/sec. The velocity field of individual features is often quite complicated; many spectral features are inclined to the direction of dispersion, implying that differential mass motions are present.
- The existence of anomalously broad H and K profiles is real. Even with high dispersion and the best seeing, such profiles are not resolved into smaller features. The central reversal in K, H and Hα appears to remain unshifted when the wings are displaced in wavelength, indicating that the reversal is non-spicular.