Hi, this is the continuation of a post... The point is that I have a file where blocks of text appear sometimes once, sometimes twice or even three times etc... I would like to find out how to delete the blocks that are repeated, so that in the end I am left with a text file in which the blocks appear only ONCE....
The text file looks like this, for instance:(please note that there are NOT blank lines in my text file, it's just after pasting here) What a call a "block" is a paragraph starting with a "<br><a href="http://xxx.lanl.gov/..."; until the next "<br><a href="http://xxx.lanl.gov/..."; <!-- comenca --> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605038";> astro-ph/0605038</a> <br> <b>Títol/<i>Title</i>:</b> The Mass of the Central Black Hole in the Seyfert Galaxy <br> NGC 4151 <br> <b>Autors:</b> Kyle G. Metzroth (1, 2), Christopher A. Onken (1,3), <br> Bradley M. Peterson (1) ((1) Department of Astronomy, The Ohio <br> State University, (2) Department of Mechanical Engineering, The <br> Ohio State University, (3) NRC Herzberg Institute of Astrophysics) <br> <b>Comentaris/<i>Comments</i>:</b> 25 pages, 5 figures. Accepted for publication in The <br> Astrophysical Journal <br> <br> In order to improve the reverberation-mapping based estimate of <br> the mass of the central supermassive black hole in the Seyfert 1 <br> galaxy NGC 4151, we have reanalyzed archival ultraviolet <br> monitoring spectra from two campaigns undertaken with the <br> International Ultraviolet Explorer. We measure emission-line time <br> delays for four lines, C IV 1549, He II 1640, C III] 1909, and Mg <br> II 2798, from both campaigns. We combine these measurements with <br> the dispersion of the variable part of each respective emission <br> line to obtain the mass of the central object. Despite the <br> problematic nature of some of the data, we are able to measure a <br> mass of 41.1 (+/- 7.3) million solar masses, although this, like <br> all reverberation-based masses, is probably systematically <br> uncertain by a factor of 3-4. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605038";> astro-ph/0605038</a> <br> <b>Títol/<i>Title</i>:</b> The Mass of the Central Black Hole in the Seyfert Galaxy <br> NGC 4151 <br> <b>Autors:</b> Kyle G. Metzroth (1, 2), Christopher A. Onken (1,3), <br> Bradley M. Peterson (1) ((1) Department of Astronomy, The Ohio <br> State University, (2) Department of Mechanical Engineering, The <br> Ohio State University, (3) NRC Herzberg Institute of Astrophysics) <br> <b>Comentaris/<i>Comments</i>:</b> 25 pages, 5 figures. Accepted for publication in The <br> Astrophysical Journal <br> <br> In order to improve the reverberation-mapping based estimate of <br> the mass of the central supermassive black hole in the Seyfert 1 <br> galaxy NGC 4151, we have reanalyzed archival ultraviolet <br> monitoring spectra from two campaigns undertaken with the <br> International Ultraviolet Explorer. We measure emission-line time <br> delays for four lines, C IV 1549, He II 1640, C III] 1909, and Mg <br> II 2798, from both campaigns. We combine these measurements with <br> the dispersion of the variable part of each respective emission <br> line to obtain the mass of the central object. Despite the <br> problematic nature of some of the data, we are able to measure a <br> mass of 41.1 (+/- 7.3) million solar masses, although this, like <br> all reverberation-based masses, is probably systematically <br> uncertain by a factor of 3-4. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605046";> astro-ph/0605046</a> <br> <b>Títol/<i>Title</i>:</b> On the viability of holistic cosmic-ray source models <br> <b>Autors:</b> J. Aublin, E. Parizot <br> <b>Comentaris/<i>Comments</i>:</b> 5 pages, 1 figure, Accepted for publication in Astronomy <br> and Astrophysics <br> <br> We consider the energy spectrum of cosmic-rays (CRs) from a purely <br> phenomenological point of view and investigate the possibility <br> that they all be produced by the same type of sources with a <br> single power-law spectrum, in E^{-x}, from thermal to ultra-high <br> energies. We show that the relative fluxes of the Galactic (GCR) <br> and extra-galactic (EGCR) components are compatible with such a <br> holistic model, provided that the index of the source spectrum be <br> x \simeq 2.23\pm 0.07. This is compatible with the best-fit <br> indices for both GCRs and EGCRs, assuming that their source <br> composition is the same, which is indeed the case in a holistic <br> model. It is also compatible with theoretical expectations for <br> particle acceleration at relativistic shocks. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605049";> astro-ph/0605049</a> <br> <b>Títol/<i>Title</i>:</b> X-rays from the Globular Cluster G1: Intermediate Mass <br> Black Hole or Low Mass X-ray Binary? <br> <b>Autors:</b> David Pooley (UC Berkeley), Saul Rappaport (MIT) <br> <b>Comentaris/<i>Comments</i>:</b> accepted to ApJL <br> <br> The globular cluster G1 (Mayall II) in M31 is the most massive <br> (~10^7 M_sun) stellar cluster in the Local Group, and it has the <br> highest central velocity dispersion (~28 km/s). It has been <br> claimed to host a central ~20,000 M_sun black hole, but these <br> claims have been controversial. We report here the XMM-Newton <br> detection of X-ray emission from G1 at a level of Lx ~ 2x10^{36} <br> erg/s. This emission could be the result of Bondi-Hoyle accretion <br> of ionized cluster gas by a central black hole, or it could be <br> produced by a conventional low-mass X-ray binary. A precise <br> localization of the X-ray emission, which is not possible with the <br> current XMM data, could distinguish between these possibilities. <br> While such a measurement may be difficult, it is of sufficient <br> potential importance to pursue. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605049";> astro-ph/0605049</a> <br> <b>Títol/<i>Title</i>:</b> X-rays from the Globular Cluster G1: Intermediate Mass <br> Black Hole or Low Mass X-ray Binary? <br> <b>Autors:</b> David Pooley (UC Berkeley), Saul Rappaport (MIT) <br> <b>Comentaris/<i>Comments</i>:</b> accepted to ApJL <br> <br> The globular cluster G1 (Mayall II) in M31 is the most massive <br> (~10^7 M_sun) stellar cluster in the Local Group, and it has the <br> highest central velocity dispersion (~28 km/s). It has been <br> claimed to host a central ~20,000 M_sun black hole, but these <br> claims have been controversial. We report here the XMM-Newton <br> detection of X-ray emission from G1 at a level of Lx ~ 2x10^{36} <br> erg/s. This emission could be the result of Bondi-Hoyle accretion <br> of ionized cluster gas by a central black hole, or it could be <br> produced by a conventional low-mass X-ray binary. A precise <br> localization of the X-ray emission, which is not possible with the <br> current XMM data, could distinguish between these possibilities. <br> While such a measurement may be difficult, it is of sufficient <br> potential importance to pursue. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605049";> astro-ph/0605049</a> <br> <b>Títol/<i>Title</i>:</b> X-rays from the Globular Cluster G1: Intermediate Mass <br> Black Hole or Low Mass X-ray Binary? <br> <b>Autors:</b> David Pooley (UC Berkeley), Saul Rappaport (MIT) <br> <b>Comentaris/<i>Comments</i>:</b> accepted to ApJL <br> <br> The globular cluster G1 (Mayall II) in M31 is the most massive <br> (~10^7 M_sun) stellar cluster in the Local Group, and it has the <br> highest central velocity dispersion (~28 km/s). It has been <br> claimed to host a central ~20,000 M_sun black hole, but these <br> claims have been controversial. We report here the XMM-Newton <br> detection of X-ray emission from G1 at a level of Lx ~ 2x10^{36} <br> erg/s. This emission could be the result of Bondi-Hoyle accretion <br> of ionized cluster gas by a central black hole, or it could be <br> produced by a conventional low-mass X-ray binary. A precise <br> localization of the X-ray emission, which is not possible with the <br> current XMM data, could distinguish between these possibilities. <br> While such a measurement may be difficult, it is of sufficient <br> potential importance to pursue. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605049";> astro-ph/0605049</a> <br> <b>Títol/<i>Title</i>:</b> X-rays from the Globular Cluster G1: Intermediate Mass <br> Black Hole or Low Mass X-ray Binary? <br> <b>Autors:</b> David Pooley (UC Berkeley), Saul Rappaport (MIT) <br> <b>Comentaris/<i>Comments</i>:</b> accepted to ApJL <br> <br> The globular cluster G1 (Mayall II) in M31 is the most massive <br> (~10^7 M_sun) stellar cluster in the Local Group, and it has the <br> highest central velocity dispersion (~28 km/s). It has been <br> claimed to host a central ~20,000 M_sun black hole, but these <br> claims have been controversial. We report here the XMM-Newton <br> detection of X-ray emission from G1 at a level of Lx ~ 2x10^{36} <br> erg/s. This emission could be the result of Bondi-Hoyle accretion <br> of ionized cluster gas by a central black hole, or it could be <br> produced by a conventional low-mass X-ray binary. A precise <br> localization of the X-ray emission, which is not possible with the <br> current XMM data, could distinguish between these possibilities. <br> While such a measurement may be difficult, it is of sufficient <br> potential importance to pursue. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605051";> astro-ph/0605051</a> <br> <b>Títol/<i>Title</i>:</b> Spitzer Reveals Infrared Optically-Thin Synchrotron <br> Emission from the Compact Jet of the Neutron Star X-Ray Binary 4U <br> 0614+091 <br> <b>Autors:</b> S. Migliari (UCSD), J.A. Tomsick (UCSD), T.J. Maccarone <br> (Southampton), E. Gallo (UCSB), R.P. Fender (Southampton), G. <br> Nelemans (Nijmegen), D.M. Russell (Southampton) <br> <b>Comentaris/<i>Comments</i>:</b> Accepted for publication in ApJ Letters <br> <br> Spitzer observations of the neutron star (ultra-compact) X-ray <br> binary (XRB) 4U 0614+091 with the Infrared Array Camera reveal <br> emission of non-thermal origin in the range 3.5-8 um. The <br> mid-infrared spectrum is well fit by a power law with spectral <br> index of alpha=-0.57+/-0.04 (where the flux density is F_nu <br> \propto nu^(alpha)). Given the ultra-compact nature of the binary <br> system, we exclude the possibility that either the companion star <br> or the accretion disk can be the origin of the observed emission. <br> These observations represent the first spectral evidence for a <br> compact jet in a low-luminosity neutron star XRB and furthermore <br> of the presence, already observed in two black hole (BH) XRBs, of <br> a `break' in the synchrotron spectrum of such compact jets. We can <br> derive a firm upper limit on the break frequency of the spectrum <br> of nu_thin=3.7x10^(13) Hz, which is lower than that observed in BH <br> XRBs by at least a factor of 10. Assuming a high-energy cooling <br> cutoff at ~1 keV, we estimate a total (integrated up to X-rays) <br> jet power to X-ray bolometric luminosity ratio of \~5%, much lower <br> than that inferred in BHs. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605059";> astro-ph/0605059</a> <br> <b>Títol/<i>Title</i>:</b> The Abundances of Light Neutron-Capture Elements in <br> Planetary Nebulae <br> <b>Autors:</b> N. C. Sterling, Harriet L. Dinerstein (University of <br> Texas at Austin) <br> <b>Comentaris/<i>Comments</i>:</b> 4 pages, 1 figure, to appear in IAU Symp. 234, <br> "Planetary Nebulae in our Galaxy and Beyond", eds. M. J. Barlow <br> and R. H. Mendez <br> <br> We present preliminary results from a large-scale survey of the <br> neutron(n)-capture elements Se and Kr in Galactic planetary <br> nebulae (PNe). These elements may be produced in PN progenitors by <br> s-process nucleosynthesis, and brought to the stellar envelope by <br> third dredge-up (TDU). We have searched for [Kr III] 2.199 and [Se <br> IV] 2.287 $\mu$m in 120 PNe, and detected one or both lines in 79 <br> objects, for a detection rate of 66%. In order to determine <br> abundances of Se and Kr, we have added these elements to the <br> atomic database of the photoionization code CLOUDY, and <br> constructed a large grid of models to derive corrections for <br> unobserved ionization stages. Se and Kr are enriched in 73% of the <br> PNe in which they have been detected, and exhibit a wide range of <br> abundances, from roughly solar to enriched by a factor of 10 or <br> more. These enrichments are interpreted as evidence for the <br> operation of the s-process and TDU in the progenitor stars. In <br> line with theoretical expectations, Kr is more strongly enhanced <br> than Se, and the abundances of both elements are correlated with <br> the carbon abundance. Kr and Se are strongly enhanced in Type I <br> PNe, which may be evidence for the operation of the $^{22}$Ne <br> neutron source in intermediate-mass AGB stars. These results <br> constitute the first broad characterization of s-process <br> enrichments in PNe as a population, and reveal the impact of low- <br> and intermediate-mass stars on the chemical evolution of <br> trans-iron elements in the Galaxy. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605059";> astro-ph/0605059</a> <br> <b>Títol/<i>Title</i>:</b> The Abundances of Light Neutron-Capture Elements in <br> Planetary Nebulae <br> <b>Autors:</b> N. C. Sterling, Harriet L. Dinerstein (University of <br> Texas at Austin) <br> <b>Comentaris/<i>Comments</i>:</b> 4 pages, 1 figure, to appear in IAU Symp. 234, <br> "Planetary Nebulae in our Galaxy and Beyond", eds. M. J. Barlow <br> and R. H. Mendez <br> <br> We present preliminary results from a large-scale survey of the <br> neutron(n)-capture elements Se and Kr in Galactic planetary <br> nebulae (PNe). These elements may be produced in PN progenitors by <br> s-process nucleosynthesis, and brought to the stellar envelope by <br> third dredge-up (TDU). We have searched for [Kr III] 2.199 and [Se <br> IV] 2.287 $\mu$m in 120 PNe, and detected one or both lines in 79 <br> objects, for a detection rate of 66%. In order to determine <br> abundances of Se and Kr, we have added these elements to the <br> atomic database of the photoionization code CLOUDY, and <br> constructed a large grid of models to derive corrections for <br> unobserved ionization stages. Se and Kr are enriched in 73% of the <br> PNe in which they have been detected, and exhibit a wide range of <br> abundances, from roughly solar to enriched by a factor of 10 or <br> more. These enrichments are interpreted as evidence for the <br> operation of the s-process and TDU in the progenitor stars. In <br> line with theoretical expectations, Kr is more strongly enhanced <br> than Se, and the abundances of both elements are correlated with <br> the carbon abundance. Kr and Se are strongly enhanced in Type I <br> PNe, which may be evidence for the operation of the $^{22}$Ne <br> neutron source in intermediate-mass AGB stars. These results <br> constitute the first broad characterization of s-process <br> enrichments in PNe as a population, and reveal the impact of low- <br> and intermediate-mass stars on the chemical evolution of <br> trans-iron elements in the Galaxy. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605066";> astro-ph/0605066</a> <br> <b>Títol/<i>Title</i>:</b> Galactic Abundance Patterns via Peimbert Types I & II <br> Planetary Nebulae <br> <b>Autors:</b> J.B. Milingo (Franklin & Marshall College), K.B. Kwitter <br> (Williams College), R.B.C. Henry (University of Oklahoma), S.P. <br> Souza (Williams College) <br> <br> Planetary Nebulae (PNe) abundance patterns have long been used to <br> note signatures of nuclear processing and to trace the <br> distribution of metals throughout galaxies. We present abundance <br> gradients and heavy element ratios based upon newly acquired <br> spectrophotometry of a sample of >120 Galactic PNe. This new data <br> set is extracted from spectra that extend from 3600 - 9600 A, <br> allowing the use of [S III] features at 9069 and 9532 A. Since a <br> significant portion of S in PNe resides in S+2 and higher <br> ionization stages, including these strong features should improve <br> the extrapolation from observed ion abundances to total element <br> abundance. S is believed to be precluded from enhancement and <br> depletion across the range of PNe progenitor masses, making it an <br> alternate metallicity tracer to the canonical oxygen. If S can be <br> reliably determined in PNe, its stability in intermediate mass <br> stars makes it a valuable tool to probe the natal conditions as <br> well as the evolution of PNe progenitors. This is a continuation <br> of our Type II PNe work, the impetus being to compile a relatively <br> large set of line strengths and abundances with internally <br> consistent observation, reduction, measurement, and abundance <br> determination, minimizing systematic effects that come from <br> compiling various data sets. This research is supported by the AAS <br> Small Research Grants program, the Franklin & Marshall Committee <br> on Grants, and NSF grant AST- 0307118. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605069";> astro-ph/0605069</a> <br> <b>Títol/<i>Title</i>:</b> A Fresh Look at the Binary Characteristics Among Massive <br> Stars with Implications for Supernova and X-Ray Binary Rates <br> <b>Autors:</b> Henry A. Kobulnicky (1), Chris L. Fryer (2), Daniel C. <br> Kiminki (1) ((1) University of Wyoming, (2) Los Alamos National <br> Laboratory) <br> <b>Comentaris/<i>Comments</i>:</b> 40 pages, 18 figures; Submitted to ApJ; comments welcome <br> <br> We use a radial velocity survey of 141 early-type stars in the <br> Cygnus OB2 Association over a 6-year time baseline to <br> statistically describe the binary properties among massive stars. <br> The observed radial velocity variations permit an estimate of the <br> binary fraction, f, the power law index of the distribution of <br> companion masses, alpha, and the power law index of orbital <br> separations, beta. We constrain f to be >0.6 and in the probable <br> range 0.7 - 1.0. Comparison of the data to populations of binary <br> systems simulated by Monte-Carlo methods indicates a firm lower <br> limit of alpha>-0.8 regardless of assumptions about the true <br> binary frequency. If f>0.9, then the data require mass ratios <br> peaked toward unity with alpha>0.0. These data indicate that the <br> mass ratios in O and early B type systems are approximately flat <br> or peaked toward unity, broadly consistent with Garmany, Conti, & <br> Massey (1980). Our analysis rules out the possibility that the <br> companions to massive stars are drawn from the field star mass <br> distribution with alpha<-2. Assuming the lowest reasonable value <br> of alpha, the classic low-mass X-ray binary formation scenario <br> falls short from producing enough of these binaries. Alternate <br> scenarios, such as those invoking intermediate mass primaries, <br> must be the dominate formation scenarios for low-mass X-ray <br> binaries. The large binary fraction poses a problem for <br> single-star progenitors for type Ib/c supernovae and strengthens <br> the case for binaries dominating the progenitors of this class of <br> supernovae. (Abridged) <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605070";> astro-ph/0605070</a> <br> <b>Títol/<i>Title</i>:</b> Dynamics of galaxy cores and supermassive black holes <br> <b>Autors:</b> David Merritt <br> <b>Comentaris/<i>Comments</i>:</b> 75 pages, 28 figures. To appear in Reports on Progress <br> in Physics <br> <br> Recent work on the dynamical evolution of galactic nuclei <br> containing supermassive black holes is reviewed. Topics include <br> galaxy structural properties; collisionless and collisional <br> equilibria; loss-cone dynamics; and dynamics of binary and <br> multiple supermassive black holes. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605070";> astro-ph/0605070</a> <br> <b>Títol/<i>Title</i>:</b> Dynamics of galaxy cores and supermassive black holes <br> <b>Autors:</b> David Merritt <br> <b>Comentaris/<i>Comments</i>:</b> 75 pages, 28 figures. To appear in Reports on Progress <br> in Physics <br> <br> Recent work on the dynamical evolution of galactic nuclei <br> containing supermassive black holes is reviewed. Topics include <br> galaxy structural properties; collisionless and collisional <br> equilibria; loss-cone dynamics; and dynamics of binary and <br> multiple supermassive black holes. <br> <br> <br> <br><a href="http://xxx.lanl.gov/pdf/astro-ph/0605070";> astro-ph/0605070</a> <br> <b>Títol/<i>Title</i>:</b> Dynamics of galaxy cores and supermassive black holes <br> <b>Autors:</b> David Merritt <br> <b>Comentaris/<i>Comments</i>:</b> 75 pages, 28 figures. To appear in Reports on Progress <br> in Physics <br> <br> Recent work on the dynamical evolution of galactic nuclei <br> containing supermassive black holes is reviewed. Topics include <br> galaxy structural properties; collisionless and collisional <br> equilibria; loss-cone dynamics; and dynamics of binary and <br> multiple supermassive black holes. <br> <br> <!-- acaba -->
