arxiv_id stringlengths 9 16 | fig_idx int64 1 406 | caption stringlengths 20 200 | citations int64 0 7.35k |
|---|---|---|---|
astro-ph/0001011 | 1 | Duration distribution of short GRBs. The solid line is the common BeppoSAX/Batse Sample distribution, the dashed one is the normalized 4B Batse distribution, for comparison. | 1 |
astro-ph/0001016 | 2 | Illustration of the two surveys strips and the distribution of spheres with radii of 1 Mpc around known galaxies (thin circles) and galaxy groups (thick circles). The grey areas indicate the Zone of A | 13 |
astro-ph/0001018 | 2 | Boxplots of sodium abundances in M13 (Pilachowski 1996b) and field giant stars (Pilachowski 1996a). The statistical abundance distributions represented by each box's vertical boundaries, etc., are a | 10 |
astro-ph/0001034 | 2 | The Oxygen VII triplet in the LETGS -1 order spectrum with the resonance (r), the forbidden (f), and the intercombination (i) line. The measured ratios of these lines (from the fitted curve) are given | 150 |
astro-ph/0001010 | 7 | {Number evolution of different objects in the simulation box for run A.} | 0 |
astro-ph/0001030 | 6 | Optical spectrum of UGC 12237. See section 5 for details. | 0 |
astro-ph/0001061 | 3 | A compilation of density fluctuations on different scales from various observations: a galaxy survey, deep radio surveys, the X-ray Background and Cosmic Microwave Background experiments. The measurem | 9 |
astro-ph/0001048 | 5 | Exclusion diagrams for companions to two different microlenses. {Left:} Companions to MACHO 98-BLG-35 are excluded in the shaded regions (Rhie et al. 2000); the larger the mass ratio, the larger the e | 0 |
astro-ph/0001075 | 8 | C IV column density distribution in Q1422+231 at $\langle z \rangle \simeq 3.15$ (reproduced from Ellison {et al.} 2000); $f$($N$) is the number of C IV systems per column density interval and per uni | 7 |
astro-ph/0001083 | 3 | Expected rate versus event timescale towards $\gsct$. Detection efficiencies $\epsilon(\Delta t)$ are taken into account. | 2 |
astro-ph/0001078 | 8 | Values of $\Gamma$ and $R$ in the hard state of BH binaries (open circles; same as in Figure 3) and neutron-star binaries (open squares), in Seyfert 1s (crosses) and broad-line radio galaxies (asteris | 6 |
astro-ph/0001087 | 3 | Color offsets $\Delta(X-V)$ or $\Delta(V-X)$ (data$-$models) for Scalo or Miller-Scalo IMF. Symbols same as Figure <ref>. The $-1.5$ and $-0.5$ bins in [Fe/H] are Worthey models; the $-1.63$ and $-0.6 | 28 |
astro-ph/0001080 | 6 | ROSAT/HRI image of A3570. a) In an image smoothed with a Gaussian of $\sigma=6\arcsec$ distinct sources dominate over the faint cluster emission. The sources A, B, C, and E are point-like while D has | 11 |
astro-ph/0001095 | 5 | Energy dependence of coherence function. The results from Observation 3 are shown, as an example. As for Fig. 4, the results are for the 8.1-13.3 keV band and derived by averaging over 0.004-0.1 Hz. | 31 |
astro-ph/0001111 | 4 | The implied fluence ($>$ 50 GeV) of very high energy emission from GRB 970417a as a function of high-energy cutoff for five assumed differential spectral indices. | 109 |
astro-ph/0001135 | 2 | A montage showing the Type I burst profile from GS 1826-238 from RXTE as well as the reprocessed optical emission (from Kong et al. 2000). The long duration of the burst is indicative of the delayed e | 37 |
astro-ph/0001117 | 8 | Sky distribution of PSCz sources without redshift, with galaxy identifications $b_J<19.5^m$ (open circles, 192 sources) and fainter than this or with no identification (crosses, 542 sources). | 19 |
astro-ph/0001129 | 3 | Critical spin frequencies of the r-mode instability. The solid line is the critical frequency set only by shear and bulk viscosities in the core (same as Fig. 1 of B. Owen's review in this volume). Th | 2 |
astro-ph/0001146 | 3 | The calculated Milky Way warp. Shown are the crossing points of two stable, test-particle orbits for two satellite-to-disk mass ratios: 0.1 (circles), and 0.2 (crosses). The central bar marks one disk | 22 |
astro-ph/0001145 | 2 | Upper limits to the differential flux of high energy neutrinos obtained by different experiments as well as upper bounds for neutrino fluxes from a number of different models. The triangle denotes the | 0 |
astro-ph/0001160 | 1 | Fast cooling (FC) synchrotron spectra from a shock injected power law electron distribution. The shape of the spectrum is determined by the ordering of the self absorption frequency, $\nu_{sa}$, with | 72 |
astro-ph/0001166 | 5 | Composite $i$ band image of the supercluster field (North is $\uparrow$ and East is $\rightarrow$). The cluster centers of CL1604+4304 and CL1604+4321 are at the bottom and top, respectively, of this | 14 |
astro-ph/0001212 | 4 | Examples of our WD 1704+481.2 spectra and the least-squares fit used to derive the orbital parameters of the binary. The spectra (which are in no particular order) are offset vertically from each othe | 1 |
astro-ph/0001229 | 2 | (a) Direct comparison of ages derived from the LDB method to ages derived from isochrone fitting to the YREC theoretical models. (b) Ratio of the LDB age to the YREC age, as a function of age. | 1 |
astro-ph/0001232 | 3 | Kinematical distances vs. CS95 distances for 30 . Estimated errors for the kinematical distances are indicated, as well as the 1:1 (solid line) and 2:1 (dashed one) relations. | 0 |
astro-ph/0001240 | 8 | Same as Figure - 7 but for the redshift $z_s = 2$. Note that the bias associated with high $\kappa(\theta_0)$ spots in the convergence field decreases as we increase the source redshift $z_s$. | 24 |
astro-ph/0001257 | 4 | Same as in Figure 3 for the case of isotropic oxygen velocity distribution. | 69 |
astro-ph/0001264 | 2 | Long-term X-ray lightcurve of NGC 5905 (filled squares, and arrows for upper limits). The flare occurred during the {ROSAT} all-sky survey (RASS). | 0 |
astro-ph/0001260 | 2 | The "structure index" (see text) as a function of galaxy luminosity. Open points are Virgo galaxies assuming $(m-M)_{Virgo} = 31.0$ and crosses are Coma cluster galaxies assuming $(m-M)_{Coma} = 34.9$ | 3 |
astro-ph/0001285 | 2 | Observed magnitude versus redshift for L$^*$ unevolving galaxy spectral energy distributions. The horizontal lines indicate the magnitude limits(5-$\sigma$ in a 2 arcsec diameter aperture) and the sur | 63 |
astro-ph/0001263 | 6 | Residuals after fitting a {warm absorber} to the {RASS} spectrum (= `steep-state' spectrum) of RXJ0134-4258. Residuals after fitting a {powerlaw} to the {pointed} PSPC data (= `flat-state' spectrum) o | 1 |
astro-ph/0001267 | 14 | {c)} Source detection radius for $\fwhm=2$ arcmins and $\tildy=6.84\times 10^{-4}$, e.g., $\lambda=1$ cm and $\qst\sigpix=1.5$ mJy. | 3 |
astro-ph/0001296 | 3 | High resolution imaging of $\NGC{6240}$ in the $\Htwo$ $v=1{\to}0$ S(1) line and the $2.15\mum$ continuum with NICMOS/HST <cit.>. | 4 |
astro-ph/0001291 | 12 | Spatial distribution of metallicity corrected $(b-r)_{{\rm corr}}$. The solid line represents the distance dependent upper color limit at $R=23^{mag}$, the dotted line is the lower limit due to the se | 6 |
astro-ph/0001313 | 5 | Evolution of Zn abundances in our models as a function of redshift $z$. Results are presented for a grid of 25 disc models, caracterised by 5 values of the disc maximal circular velocity V$_C$ (80, 1 | 37 |
astro-ph/0001301 | 5 | Energy flux spectrum of Cas A in . The full and the dotted curve correspond to the inferred IC emission, for a magnetic field strength $B_1$ in the bright compact radio knots, given by $B_1=1 {\rm mG~ | 2 |
astro-ph/0001325 | 1 | A region taken from the public release of the HDF-S (Williams et al. 1999). It shows the lens galaxy, the arc to its NW, and the dot to its NE. The figure measures $3\farcs2$ on a side. | 0 |
astro-ph/0001328 | 1 | (Upper panels) Radial column density profiles and $1\sigma$ errors obtained from deprojection analysis of PSPC spectra for fits over 0.2-2.2 keV (solid line), 0.5-2.2 keV (dashed), and over 0.2-2.2 ke | 14 |
astro-ph/0001347 | 3 | Similar to Fig. 2, but for a low-density CDM model with $\om=0.3$ and $\ov=0.7$. In both panels, the solid curves are computed from the original simulation particles. The dotted curve tracing the soli | 45 |
astro-ph/0001370 | 1 | Speckle-holographic power spectrum, phase, and image of the T Tauri IRC. They have been rotated to standard orientation, with North up and East left. The power and phase show the striping pattern char | 87 |
astro-ph/0001373 | 5 | A tight representation of the best fit {photometric plane}. The filled circles represent elliptical galaxies and the open circles represent bulges of disk galaxies. The line is a plane fit to the data | 45 |
astro-ph/0001372 | 4 | The same as figure 3 but for the almost quadrupole magnetic field and $i = 90^{\circ}$ and $\beta = 50^{\circ}$. The value of $i$ has been chosen so that it is consistent with $R \simeq 6.5 R_\odot$, | 32 |
astro-ph/0001378 | 6 | Determination of $c_1$, HP2, and KP from photometric, moderate resolution ($\sim 5$ Å) spectra obtained with EMMI attached to the 3.5 m ESO NTT. Dashed lines in the lower two panels indicate continuu | 1 |
astro-ph/0001393 | 3 | {Parameter Estimation} This figure shows the $\chi ^2$ surface for the $\Omega_0 - w$ parameter space of a family of spatially flat models with constant $\Omega_0 h^2$. These constraints are due to cr | 61 |
astro-ph/0001394 | 7 | Fraction of radio-loud quasars as function of redshift. Two redshift ranges are plotted. No redshift dependence in the radio-loud fraction is evident. | 81 |
astro-ph/0001382 | 20 | AMRs from Edv93 (crosses) and from this work (open circles). The major differences correspond to two areas in this diagram where we have found no stars, while Edv93 found some. These regions were name | 20 |
astro-ph/0001423 | 2 | 45$\times$45 ACIS image of the region around (left panel). The image was smoothed with a Gaussian of $\sigma$=2. The cross marks the optical position of the Be star identified by Hughes & Smith (199 | 16 |
astro-ph/0001433 | 2 | The electron spectrum in the center of the Coma cluster (from Enßlin & Biermann 1998). The solid line below 1 MeV$/c$ is the thermal electron spectrum and the lines around 1 GeV$/c$ give the radio emi | 0 |
astro-ph/0001413 | 4 | The FBLF from <cit.>, reproduced from their Figure 5 after converting to $H_0=75\,$kms$^{-1}$Mpc$^{-1}$ and 1.4 GHz (solid symbols). The open symbols show the FBLF calculated for A2877. Error bars hav | 9 |
astro-ph/0001434 | 1 | Evolution of theoretical isochrones for solar metallicities ($Z=0.019$). They are derived from the Girardi et al. (2000; for $M\le7$ ) and Bertelli et al. (1994; for $M>7$ ) databases of stellar track | 3 |
astro-ph/0001436 | 8 | X-ray (2-10 keV) light curves of a sample of afterglows by BeppoSAX | 1 |
astro-ph/0001456 | 1 | Pulsar sensitivity curves for DMs of 0, 100, and 500 pc cm$^{-3}$, assuming a 5% intrinsic pulsed duty cycle. The dashed horizontal line at 58 mJy is the flux density of our weakest source at 600 MHz, | 17 |
astro-ph/0001465 | 4 | Left: R-band light curve of GRB 980326 and the sum of an initial power-law decay plus Ic supernova light curve for redshifts ranging from $z = 0.50$ to $z=1.60$ (from [40]). Right: The broad-band spec | 1 |
astro-ph/0001461 | 2 | Average spectrum obtained from a set of 28 galaxies, including the galaxies in Figure 1 (3). The quantities plotted are the same as those in Fig. 1, except for the use of logarithmic scales on both ax | 101 |
astro-ph/0001469 | 6 | Same as Fig. <ref> for simulated SNe in the LCDM model. Multiple images are displayed with circle dots; note that both magnified and de-magnified images are present in multiple systems. | 11 |
astro-ph/0001483 | 14 | Integrated properties of our models at an age T=13.5 Gyr. Mass of stars ({top left}), mass of gas ({middle left}), gas fraction ({bottom left}), M/L values in B- and I- bands ({top center}), average o | 0 |
astro-ph/0001504 | 4 | Pisces AGN Group (filled squares) at $z=0.267\pm0.033$. The two objects to the right are in the same redshift range but their relation to the group is unknown. AGN in front of (large squares) and behi | 3 |
astro-ph/0001496 | 4 | Schematic Description of Lens Model a) Source plane. Source points within the astroid caustic are associated with four image points around the Einstein ring with similar intensity (ignoring an unobser | 6 |
astro-ph/0001459 | 1 | A histogram showing the criterion used to exclude 5 radio-loud sources from the Seyfert sample. The frequency of sources per logarithmic radio to far-infrared luminosity ratio interval $\Delta$log(L$_ | 100 |
gr-qc/0001061 | 1 | Left: Mass $M$ and particle number $N$ (or rest mass $mN$ at infinity) of a BS depending on the central density $\rho$. Right: Mass-radius dependence of an axionic BS. | 112 |
hep-ph/0001168 | 2 | The total equation of state $w_{\text{total}} = P_{\text{pngb}}/( \protect\rho_{\text{matter}}+\protect\rho_{\text{pngb}})$ and the PNGB equation of state $w_{\text{pngb}} = P_{\text{pngb}}/\protect\r | 14 |
astro-ph/0002003 | 6 | The central region of the Fornax Cluster with the positions of the new compact objects indicated by squares. This R-band photographic image is from a single UKST exposure on Tech-Pan emulsion, digitis | 204 |
astro-ph/0002031 | 1 | The formation epoch of objects with various masses in a standard CDM model ($\Omega=n=\sigma_{8h^{-1}}=1$), shown as a fraction of the current age of the universe. The upper labels indicate redshifts. | 7 |
astro-ph/0002037 | 7 | The power spectrum quadrupole to monopole ratio $\Delta_2/\Delta_0$ as a function of scale for scale-free initial spectra $n=-1.4$ for Gaussian (squares) and $\chi^2$ initial conditions (triangles). T | 35 |
astro-ph/0002046 | 5 | Model results for the dust components in IIZw40 (left) and NGC 1569 (right) fitted to the ISOCAM MIR spectra and the IRAS data (boxes) Component are from the Désert et al. model <cit.> (see text for | 108 |
astro-ph/0002053 | 3 | Evaporation rate ${\dot M(r)}$ as in Fig. 2. Inward extension of the standard thin disk for 3 different mass flow rates ${\dot M}$ in the thin disk (schematic). Note that the standard thin disk reache | 0 |
astro-ph/0002030 | 24 | The power spectra in CDM fluctuations predicted by cosmic strings, sCDM, and by inflation and strings with $R_{\rm{SI}}=0.25,0.5,0.75.$ We have also superposed the power spectrum as inferred from surv | 14 |
astro-ph/0002098 | 5 | {Left:} Abundance of HCN, $N$(HCN)/$N_{\rm tot}$(H$_2$), as a function of the $^{13}$CO excitation temperature measured by Mitchell et al. (1990). {Middle:} Abundance of H$_2$O in the warm gas $N$(H$_ | 5 |
astro-ph/0002083 | 10 | Spectral Energy Distributions | 175 |
astro-ph/0002116 | 3 | Original and final IPN error boxes for GRB991208 (3 $\sigma$ confidence). The original error box (Hurley et al. 1999) is drawn with dashed lines. The final error box is defined by the intersection of | 31 |
astro-ph/0002113 | 2 | Visual interactive user interfaces, based on graph edges. Vertices are author names, article titles and (not shown here) astronomical object names. Map for astronomer Jean Heyvaerts. Original in color | 3 |
astro-ph/0002117 | 2 | {left)} Effects of pulse scattering on time series and power spectrum when modeled as by CL97 and when applying the actual formulae, {right)} scattered pulsed flux for a model pulsar of $P=1$ s and a | 2 |
astro-ph/0002112 | 8 | {a-c.} Accuracy of the third order approximation for power-law medium, $\gamma=5/3$ and $N=2$: a relative differences for $m=-4$, b relative differences for $m=-2$, c relative differences for $m=1$. L | 5 |
astro-ph/0002093 | 5 | Doppler map prepared based on two-dimensional calculation; a): \( \gamma \) = 1.01 b): \( \gamma \) = 1.2 | 10 |
astro-ph/0002136 | 8 | The galaxy number count predictions at assumed IRIS two bandpasses (N60 and N170). The dot-dashed lines denote the IRIS Far-infrared Scanner (FIS) flux detection limit at each waveband. | 2 |
astro-ph/0002162 | 2 | Likelihood contours for $l$ vs $\delta T_l$ for the position of the peak. For BOOM/NA and TOCO, we use the stretch method using RADPACK<cit.> and include the calibration error. For Previous and ALL (t | 50 |
astro-ph/0002156 | 5 | A schematic picture of a pocket universe, illustrating Vilenkin's proposal for the calculation of probabilities. | 263 |
astro-ph/0002166 | 5 | HRC radial intensity distributions around the point-like emission peak of . The pulsar radial profile (solid line) is consistent with the HRC point-spread function. The nebula profile (dotted line) is | 57 |
astro-ph/0002165 | 5 | Left: Shape of the emitting region. Dash line marks the physical extent of the jet while solid lines give the viewable region $1/\gamma$. The observed radiation is coming from the gray region. On each | 1 |
astro-ph/0002181 | 4 | (a) Plot of lognormal mean waiting times till the next burst ($\Delta$$T^{+}$) vs mean total counts. No correlation is seen ($\rho$ = $-$0.2, P=0.70); (b) The plot of lognormal mean elapsed times sinc | 107 |
astro-ph/0002183 | 7 | The continuous line represents the evolution of the space density of quasars with $M_B < -24$ predicted by the $\Lambda$CDM model described in the text (KH99). Filled circles are data from the present | 31 |
astro-ph/0002168 | 9 | {Left: Radio afterglow of GRB 980329 <cit.>. The rapid rise of the centimeter flux and the high absorption frequency (signified by the considerable strength of the millimeter emission) offer good supp | 19 |
astro-ph/0002212 | 2 | The proposed atmospheric structure of $\eta$ Carinae during its great eruption. A homogeneous atmosphere is unstable as a result of two generic instabilities that take place even in Thomson atmosphere | 91 |
astro-ph/0002220 | 7 | The X-ray luminosity and pulse fraction of the AXPs and SGRs are plotted against the magnetic field strength assuming that these objects are magnetars. Two values of the luminosity are plotted for to | 138 |
astro-ph/0002226 | 2 | (a) Color versus mass-to-luminosity ratio for a variety of galaxy types (from OBS). (b) Galaxies from the sample of OBS. The solid and dashed lines are the 1$\sigma$ and 2$\sigma$ fits to the LSB gala | 0 |
astro-ph/0002246 | 2 | $I,I-Z$ diagram for all of the objects in our observed fields. The L-dwarfs are indicated by circles with error bars and the other objects by crosses. Note that the photometry is based on a single obs | 0 |
astro-ph/0002253 | 2 | 95% C.L. exclusion diagram on the halo mass fraction in the form of compact objects of mass $M$, for the standard halo model ($4 \times 10^{11}\:{\rm M}_\odot$ inside 50 kpc), from all and data 199 | 43 |
astro-ph/0002258 | 9 | Examples of $4\times 4$ $M=1$ surveys on square (1st and 2nd rows), staggered (middle row), and triangular grids (4th and 5th rows) for various angles between the detector array and the grid orientati | 25 |
astro-ph/0002266 | 7 | The interstellar reddening map of M81, using the method described in the text. | 64 |
astro-ph/0002296 | 2 | As Figure 1, but for $N_{\nu} = 3.2$ | 2 |
astro-ph/0002306 | 1 | Radiation transfer effects on GRB emission that passes through electrons energized by an earlier portion of the photon front. The intrinsic spectrum eq.(1), with $\alpha_X = 2/3$, $\alpha_\gamma = 2.5 | 25 |
astro-ph/0002308 | 1 | Panel (a) is a view of the central 32 Mpc region of our SIDM simulation at a redshift z=0. Panel (b) shows the velocity vectors of particles within the central 500 kpc of one of the SIDM halos. The sy | 88 |
astro-ph/0002320 | 2 | {A:} Arecibo image of CHVC $158\!-\!39\!-\!285$ showing at 3 arcmin resolution; contours are drawn at levels of 5, 10, 20, and $30 \times 10^{18}$ cm$^{-2}$. {B:} Intensity-weighted line-of-sight vel | 0 |
astro-ph/0002323 | 5 | Fractional infrared luminosity versus age. Early-type Vega-like stars are plotted as solid circles and late-type Vega-like stars are plotted as filled diamonds. Field K stars with IR excess upper limi | 59 |
astro-ph/0002333 | 3 | Trend of the broad band magnitudes of HE 0512$-$3329 for components A, B, and the composite A+B. The VRI photometry is from the ground-based CTIO imaging while the B magnitudes are derived from the di | 21 |
astro-ph/0002339 | 1 | Wind evolution towards a stationary, overloaded solution showing an extended decelerating region. A periodic sawtooth perturbation is introduced into a shallow solution at $z=0.8$, upstream from the c | 15 |
astro-ph/0002338 | 2 | Spectrum of 300 at $z = 5.50$, obtained with LRIS on the Keck II telescope. The total exposure time is 4.5 hours, and the spectrum was extracted using a 15 $\times$ 15 aperture. The spectrum has been | 20 |
astro-ph/0002340 | 3 | The image on the left shows the core of the cluster (A) and a possibly associated group (B). The central and right panels show the surface density of galaxies in a {much larger region} (roughly 20'x30 | 1 |
astro-ph/0002360 | 3 | The matter power spectrum from the TOE model of Figure <ref>. Also shown is a cosmological constant model with all other parameters equal. Power is significantly smaller in the TOE model. | 125 |
astro-ph/0002336 | 5 | The middle panel shows the likelihood contours for a fixed $h=0.65$ in the X-ray survey, as in Figure <ref>. The left and right panels show the deviations in the contours caused by a $\pm 2\%$ offset | 364 |
End of preview. Expand in Data Studio
No dataset card yet
- Downloads last month
- 34