We present JWST/NIRSpec PRISM follow-up of candidate galaxies at z=9-11 selected from deep JWST/NIRCam photometry in GLASS-JWST Early Release Science data. We spectroscopically confirm six sources with secure redshifts at z = 9.52-10.43, each showing multiple emission lines. An additional object is likely at z = 10.66, based on its Lya-break and a single emission feature, while one source is a lower redshift interloper. The sample includes the first JWST-detected candidate at z=10, GHZ1/GLASS-z10, which we confirm at z = 9.875, and the X-ray detected AGN GHZ9 confirmed at z = 10.145. Three objects in our sample, including GHZ9, have EW(CIII])>20A and occupy a region compatible with AGN emission in the EW(CIII]) vs CIV/CIII] diagram. The spectroscopic sample confirms a high abundance of galaxies at z > 9. We measure a number density of z=10 galaxies in the GLASS-JWST ERS field that is a factor of >3 higher than other JWST-based estimates at demagnified rest-frame magnitudes of -21 < Muv < -19. We find that the positions of these galaxies in redshift and angular space are not consistent with all of them being part of a unique progenitor of present-day galaxy clusters. The high density of objects in the GLASS region can be explained either by clustering on large scales or by a superposition of different forming structures of which we observe only the brightest members. By considering all the spectroscopic z=10 sources in the Abell-2744 field, we identify two potential galaxy proto-clusters centered around GHZ9 and JD1, with relative separations between their members of 1-2 pMpc. The potential AGN nature of three of the sources in our sample lends support to a scenario in which the high abundance of bright sources determined by JWST surveys at cosmic dawn may be affected by AGN contribution to their UV luminosity.

Self-interacting dark matter (SIDM) arises generically in scenarios for physics beyond the Standard Model that have dark sectors with light mediators or strong dynamics. The self-interactions allow energy and momentum transport through halos, altering their structure and dynamics relative to those produced by collisionless dark matter. SIDM models provide a promising way to explain the diversity of galactic rotation curves, and they form a predictive and versatile framework for interpreting astrophysical phenomena related to dark matter. This review provides a comprehensive explanation of the physical effects of dark matter self-interactions in objects ranging from galactic satellites (dark and luminous) to clusters of galaxies and the large-scale structure. The second major part describes the methods used to constrain SIDM models including current constraints, with the aim of advancing tests with upcoming galaxy surveys. This part also provides a detailed review of the unresolved small-scale structure formation issues and concrete ways to test simple SIDM models. The review is rounded off by a discussion of the theoretical motivation for self-interactions, degeneracies with baryonic and gravitational effects, extensions to the single-component elastic-interactions SIDM framework, and future observational and theoretical prospects.

Understanding how galaxies quench their star formation is crucial for studies of galaxy evolution. Quenching is related to the cold gas decrease. In the first paper we showed that the dust removal timescale in early-type galaxies (ETGs) is about 2.5 Gyr. Here we present carbon monoxide (CO) and 21 cm hydrogen (H I) line observations of these galaxies and measure the timescale of removal of the cold interstellar medium (ISM). We find that all the cold ISM components (dust, molecular and atomic gas) decline at similar rates. This allows us to rule out a wide range of potential ISM removal mechanisms (including starburst-driven outflows, astration, a decline in the number of asymptotic giant branch stars), and artificial effects like stellar mass-age correlation, environmental influence, mergers, and selection bias, leaving ionization by evolved low-mass stars and ionization/outflows by supernovae Type Ia or active galactic nuclei as viable mechanisms. We also provide evidence for an internal origin of the detected ISM. Moreover, we find that the quenching of star formation in these galaxies cannot be explained by a reduction in gas amount alone, because the star formation rates (SFRs) decrease faster (on a timescale of about 1.8 Gyr) than the amount of cold gas. Furthermore, the star formation efficiency of the ETGs (SFE = SFR/MH2) is lower than that of star-forming galaxies, whereas their gas mass fractions (fH2 = MH2/M*) are normal. This may be explained by the stabilization of gas against fragmentation, for example due to morphological quenching, turbulence, or magnetic fields.

Substantial populations of massive quiescent galaxies at $z\ge3$ challenge our understanding of rapid galaxy growth and quenching over short timescales. In order to piece together this evolutionary puzzle, more statistical samples of these objects are required. Established techniques for identifying massive quiescent galaxies are increasingly inefficient and unconstrained at $z>3$. As a result, studies report that as much as 70\% of quiescent galaxies at $z>3$ may be missed from existing surveys. In this work, we propose a new empirical color selection technique designed to select massive quiescent galaxies at $3\lesssim z \lesssim 6$ using JWST NIRCam imaging data. We use empirically-constrained galaxy SED templates to define a region in the $F277W-F444W$ vs. $F150W-F277W$ color plane that captures quiescent galaxies at $z>3$. We apply this color selection criteria to the Cosmic Evolution Early Release Science (CEERS) Survey and identify 44 candidate $z\gtrsim3$ quiescent galaxies. Over half of these sources are newly discovered and, on average, exhibit specific star formation rates of post-starburst galaxies. We derive volume density estimates of $n\sim1-4\times10^{-5}$\,Mpc$^{-3}$ at $3<z<5$, finding excellent agreement with existing reports on similar populations in the CEERS field. Thanks to NIRCam's wavelength coverage and sensitivity, this technique provides an efficient tool to search for large samples of these rare galaxies.

Infrared (IR), sub-millimetre (sub-mm) and millimetre (mm) databases contain a huge quantity of high quality data. However, a large part of these data are photometric, and are thought not to be useful to derive a quantitative information on the nebular emission of galaxies. The aim of this project is first to identify galaxies at z > 4-6, and in the epoch of reionization from their sub-mm colours. We also aim at showing that the colours can be used to try and derive physical constraints from photometric bands, when accounting for the contribution from the IR fine structure lines to these photometric bands. We model the flux of IR fine structure lines with CLOUDY, and add them to the dust continuum emission with CIGALE. Including or not emission lines in the simulated spectral energy distribution (SED) modifies the broad band emission and colours. The introduction of the lines allows to identify strong star forming galaxies at z > 4 - 6 from the log10 (PSW_250um/PMW_350um) versus log10 (LABOCA_870um/PLW_500um) colour-colour diagramme. By comparing the relevant models to each observed galaxy colour, we are able to roughly estimate the fluxes of the lines, and the associated nebular parameters. This method allows to identify a double sequence in a plot built from the ionization parameter and the gas metallicity. The HII and photodissociation region (PDR) fine structure lines are an essential part of the SEDs. It is important to add them when modelling the spectra, especially at z > 4 - 6 where their equivalent widths can be large. Conversely, we show that we can extract some information on strong IR fine structure lines and on the physical parameters related to the nebular emission from IR colour-colour diagrams.

We report a non-detection of the [OI] 63-um emission line from the z = 6.03 galaxy G09.83808 using ALMA Band 9 observations, refuting the previously claimed detection with APEX by (Rybak et al. 2020); the new upper limit on the [OI] 63-um flux is almost 20-times lower. [OI] 63-um line could be a powerful tracer of neutral gas in the Epoch of Reionisation: yet our null result shows that detecting [OI] 63-um from z≥6 galaxies is more challenging than previously hypothesised.

Self-interacting dark matter (SIDM) offers the potential to mitigate some of the discrepancies between simulated cold dark matter (CDM) and observed galactic properties. We introduce a physically motivated SIDM model to understand the effects of self interactions on the properties of Milky Way and dwarf galaxy sized haloes. This model consists of dark matter with a nearly degenerate excited state, which allows for both elastic and inelastic scattering. In particular, the model includes a significant probability for particles to up-scatter from the ground state to the excited state. We simulate a suite of zoom-in Milky Way-sized N-body haloes with six models with different scattering cross sections to study the effects of up-scattering in SIDM models. We find that the up-scattering reaction greatly increases the central densities of the main halo through the loss of kinetic energy. However, the physical model still results in significant coring due to the presence of elastic scattering and down-scattering. These effects are not as apparent in the subhalo population compared to the main halo, but the number of subhaloes is reduced compared to CDM.

We study the effects of inelastic dark matter self-interactions on the internal structure of a simulated Milky Way (MW)-size halo. Self-interacting dark matter (SIDM) is an alternative to collisionless cold dark matter (CDM) which offers a unique solution to the problems encountered with CDM on sub-galactic scales. Although previous SIDM simulations have mainly considered elastic collisions, theoretical considerations motivate the existence of multi-state dark matter where transitions from the excited to the ground state are exothermic. In this work, we consider a self-interacting, two-state dark matter model with inelastic collisions, implemented in the Arepo code. We find that energy injection from inelastic self-interactions reduces the central density of the MW halo in a shorter timescale relative to the elastic scale, resulting in a larger core size. Inelastic collisions also isotropize the orbits, resulting in an overall lower velocity anisotropy for the inelastic MW halo. In the inner halo, the inelastic SIDM case (minor-to-major axis ratio $s \equiv c/a \approx 0.65$) is more spherical than the CDM ($s \approx 0.4$), but less spherical than the elastic SIDM case ($s \approx 0.75$). The speed distribution $f(v)$ of dark matter particles at the location of the Sun in the inelastic SIDM model shows a significant departure from the CDM model, with $f(v)$ falling more steeply at high speeds. In addition, the velocity kicks imparted during inelastic collisions produce unbound high-speed particles with velocities up to 500 km s$^{-1}$ throughout the halo. This implies that inelastic SIDM can potentially leave distinct signatures in direct detection experiments, relative to elastic SIDM and CDM.

We study evolution of self-interacting dark matter subhalos in the Milky Way tidal field. The interaction between the subhalos and the Milky Way's tides lead to more diverse dark matter distributions in the inner region, compared to their cold dark matter counterparts. We test this scenario with two Milky Way satellite galaxies, Draco and Fornax, opposite extremes in the inner dark matter content, and find that they can be accommodated within the self-interacting dark matter model proposed to explain the diverse rotation curves of spiral galaxies in the field.

An important aspect of quenching star formation is the removal of the cold interstellar medium (ISM; non-ionised gas and dust) from a galaxy. In addition, dust grains can be destroyed in a hot or turbulent medium. The adopted timescale of dust removal usually relies on uncertain theoretical estimates. It is tricky to track the dust removal, because usually dust is constantly replenished by consecutive generations of stars. Our objective is to measure observationally the timescale of dust removal. We here explore an approach to select galaxies which do have detectable amounts of dust and cold ISM but exhibit a low current dust production rate. Any decrease of the dust and gas content as a function of the age of such galaxies therefore must be attributed to processes governing the ISM removal. We used a sample of galaxies detected by Herschel in the far-infrared with visually assigned early-type morphology or spirals with red colours. We also obtained JCMT/SCUBA-2 observations for five of them. We discovered an exponential decline of the dust-to-stellar mass ratio with age, which we interpret as an evolutionary trend of dust removal from these galaxies. For the first time we directly measure the dust removal timescale in such galaxies to be tau=(2.5+-0.4) Gyr (the corresponding half-life time is (1.75+-0.25) Gyr). This quantity may be used in models in which it must be assumed a priori and cannot be derived. Any process which removes dust in these galaxies, such as dust grain destruction, cannot happen on shorter timescales. The timescale is comparable to the quenching timescales found in simulations for galaxies with similar stellar masses. The dust is likely of internal, not external origin. It was either formed in the past directly by supernovae, or from seeds produced by SNe and with grain growth in the ISM contributing substantially to the dust mass accumulation.

Zavala, Jorge A.; Montaña, Alfredo; Hughes, David H.; Yun, Min S.; Ivison, R. J.; Valiante, Elisabetta; Wilner, David; Spilker, Justin; Aretxaga, Itziar; Eales, Stephen; Avila-Reese, Vladimir; Chávez, Miguel; Cooray, Asantha; Dannerbauer, Helmut; Dunlop, James S.; Dunne, Loretta; Gómez-Ruiz, Arturo I.; Michałowski, Michał J.; Narayanan, Gopal; Nayyeri, Hooshang; Oteo, Ivan; Rosa González, Daniel; Sánchez-Argüelles, David; Schloerb, F. Peter; Serjeant, Stephen; Smith, Matthew W. L.; Terlevich, Elena; Vega, Olga; Villalba, Alan; van der Werf, Paul; Wilson, Grant W. and Zeballos, Milagros (2018). A dusty star-forming galaxy at z = 6 revealed by strong gravitational lensing. Nature Astronomy, 2(1) pp. 56–62.

Context.An important aspect of quenching star formation is the removal of the cold interstellar medium (ISM; non-ionised gas and dust) from a galaxy. In addition, dust grains can be destroyed in a hot or turbulent medium. The adopted timescale of dust removal usually relies on uncertain theoretical estimates. It is tricky to track dust removal because the dust is constantly being replenished by consecutive generations of stars.Aims.Our objective is to carry out an observational measurement of the timescale of dust removal.Methods.We explored an approach to select galaxies that demonstrate detectable amounts of dust and cold ISM coupled with a low current dust production rate. Any decrease of the dust and gas content as a function of the age of such galaxies must, therefore, be attributed to processes governing ISM removal. We used a sample of the galaxies detected byHerschelin the far-infrared with visually assigned early-type morphology or spirals with red colours. We also obtained JCMT/SCUBA-2 observations for five of these galaxies.Results.We discovered an exponential decline of the dust-to-stellar mass ratio with age, which we interpret as an evolutionary trend for the dust removal of these galaxies. For the first time, we have directly measured the dust removal timescale for such galaxies, with a result ofτ = (2.5 ± 0.4) Gyr (the corresponding half-life time is (1.75 ± 0.25) Gyr). This quantity may be applied to models in which it must be assumed a priori and cannot be derived.Conclusions.Any process which removes dust in these galaxies, such as dust grain destruction, cannot happen on shorter timescales. The timescale is comparable to the quenching timescales found in simulations for galaxies with similar stellar masses. The dust is likely of internal, not external origin. It was either formed in the past directly by supernovae (SNe) or from seeds produced by SNe, and with grain growth in the ISM contributing substantially to the dust mass accumulation.

We present the science case for mapping several thousand galaxy (proto)clusters at z=1-10 with a large aperture single dish sub-mm facility, producing a high-redshift counterpart to local large surveys of rich clusters like the well-studied Abell catalogue. Principal goals of a large survey of distant clusters are the evolution of galaxy clusters over cosmic time and the impact of environment on the evolution and formation of galaxies. To make a big leap forward in this emerging research field, the community would benefit from a large-format, wide-band, direct-detection spectrometer (e.g., based on MKID technology), covering a wide field of ~1 square degree and a frequency coverage from 70 to 700 GHz.

, The discovery of a population of high-redshift dusty star-forming galaxies through the opening of the submillimeter and millimeter wavelength windows (e.g. Smail et al. 1997; Barger et al. 1998; Hughes et al. 1998) continues to have a profound impact on our understanding of galaxy formation and evolution. These submillimeter-selected galaxies (SMGs), which are characterized by large star formation rates, contribute significantly to the total cosmic star formation rate density and to the cosmic infrared background. These galaxies have also been associated with the formation of proto-clusters and are considered to be the progenitors of local massive elliptical galaxies (see review by Casey et al. 2014). However, our knowledge of the physical properties of these galaxies and the prevalence of dust-obscured star formation at earlier epochs is completely unconstrained due to the lack of large samples of distant dusty star-forming galaxies. The largest (sub-)millimeter surveys, such as those carried out by Herschel, Planck, and the The emergence of submillimetre (submm) astronomy has led to the discovery of a cosmologically important population of submm galaxies (SMGs) that appear to be among the earliest and most actively star-forming galaxies in the Universe. While sin-gle-dish observations of SMGs have been able to greatly increase our knowledge about the evolution of star formation in the Universe (e.g., Magnelli et al. 2013; Gruppioni et al. 2013; Swinbank et al. 2014; Koprowski et al. 2017), there remain unanswered questions arising from the lack of resolution (typically between 10˝ and 30˝) at these wavelengths. How are their extreme lumi-nosities sustained, and how important are mergers? Fully resolving the submm emission directly was not possible until the leap in continuum sensitivity provided by new submm interferometers and wide-bandwidth correlators. However, finding the rarest and most massive SMGs that really push our models is far too time consuming and expensive with submm interferome-try. To circumvent this issue, interferometers can be used to fol-low-up the brightest sources detected in large single-dish submm surveys (Barger et al. 2012; Smolčić et al. 2012b; Hodge et al. Magneto-hydrodynamical models have shown that the outcome of protostellar collapse can be strongly affected by the presence of magnetic fields (Galli et al. 2006; Li et al. 2014). Their role, however, still needs to be better quantified observationally. Class 0 protostars are ideal targets to study the role of these magnetic fields during the accretion processes as it is during that phase that most of the accretion occurs (André et al. 1993; André et al. 2000). Observations of the dust polarized emission is commonly used to probe the magnetic field morphology, as non-spher-ical dust grains align preferentially to the local magnetic field. During the last 10 years, polarization observations have been carried out in order to characterize the magnetic field topology at protostellar envelope scales (Girart et al. 2006; Rao et al. 2009; Hull et al. 2014). By comparing the large and small scale B fields of protostars at 1 mm, Hull et al. (2014) find for instance that sources with higher fractional polarizations have consistent large and small scale magnetic field orientations, which could be a signature of the regulating role of magnetic fields during the infall of the protostellar core. No systematic relation, however, has been demonstrated between the core magnetic field direction and the outflow orientation (Curran & Chrysostomou 2007; Hull et al. 2013; Zhang et al. 2014). We obtained observations of the 0.87 mm polarized dust continuum for a sample of 12 Class 0 (single and multiple systems) protostars with the SMA interferometer. These observations give us access to the magnetic field morphology on 750-2000 au scales. The 0.87mm dust Empirical star formation relations that describe the conversion from gas into stars are fundamental to astronomy. To date, such relations have largely been calibrated through detailed studies of star-forming regions in the disc of the Milky Way and nearby galaxies. However, these regions are typically very similar in terms of their environmental conditions. If we wish to apply star formation relations to the vastly differing environments that are found throughout the Universe, then it is crucial that we test their validity in regions with significantly different environmental conditions. Sensitive searches are steadily adding to the number of planetesimal belts around nearby stars – analogues of our Kuiper belt – showing CO line emission, now comprising 15 systems (e.g. Moor et al. 2017). The wide range of ages for these belt-hosting systems advocates for this CO gas to be produced by release from icy exocomets. This exocomet scenario has been confirmed as the origin of the observed CO gas in four systems (Marino et al. 2016, 2017, Matrà et al. 2017a,b), where CO molecules are continuously released by cometary outgassing and then rapidly destroyed by UV radiation. This has allowed linking the observed CO gas mass to the exocometary CO content (Matrà et al. 2015), which already indicates a strong similarity between exocomets and Solar System comets (Matrà et al. 2017b). between and outgassing CO, CN, HCN, HCO The young (30 Myr) and nearby (40.4 pc) A-type star HR 8799 is the host of the first (and so far only) directly imaged multiple planet system. Near-infrared images show four companions with projected separations of 14, 24, 38, and 68 AU (Marois et al. 2008, 2010), and their orbital motions have been tracked for more than a decade (e.g. Bowler 2016). Comparison of infrared photometry with standard evolutionary models suggests these companions have masses in the range of 5 to 10 Jupiter masses (Marley et al. 2012), consistent with various dynamical calculations that im-ply masses less than 10 Jupiter masses for stability at the system age. In addition to these planetary mass companions, HR 8799 also hosts a debris disk first detected by IRAS. Multi-wavelength studies show that the debris consists of a warm (T~150 K) inner belt and a cold (T~35 K) outer belt that bracket the orbits of the directly imaged planets, plus a halo of small grains that extend to radii beyond 1000 AU (Su et al. 2009). Since millimeter emission selectively reveals the large dust grains less affected by radiative forces that trace best the parent planetesimals, we used the SMA to obtain new observations at 1.3 mm that improve on previous attempts. Wilner et al. (2018) provide a full description of this work. Submillimeter photometry marks the HR 8799 debris disk as one of the most known, at about 0.1 Earth masses (Williams and Andrews 2006), but has Single dish at 350 microns (9 arcsec resolved from cold belt star, tentative (Patience JCMT 450 and 850 microns (8 13 arcsec The Submillimeter Array (SMA) participated in the April 2018 Event Horizon Telescope (EHT) observing campaign with SWARM running at the full targeted EHT bandwidth, implementing a double sideband phased array for the very first time. With a recording data rate of 64 gigabits-per-second (Gbps) the SMA station alone produced about a petabyte of recorded phased array data over the six EHT observing tracks. Not only this, but the SMA, SWARM and the SWARM VLBI Digital Back Ends (SDBE) operated without a technical hitch over the campaign— apart from a slight weather delay on the first night—with the full data rate uniformly recorded. This picture is from SMAOC Log #8780: "Here is a photo of our software leader trying to dislodge ice from the correlator AC duct. This action is required before correlator software work can resume after snowy weather. If someone spent a day and rigged up a simple three-sided sheet metal shroud, I believe his time could be spent more profitably for the project." involved choosing and building on CASPER's designs make a wideband correlator. as the two were successfully together. roles and between grain-surface and synthesis of single-dish and interferometric radio observations and chemical network models, including the role of shocks, molecular families with multiple formation routes, isotopologue chemistry, and dust-grain precursors. The SMA is a pioneering radio interferometer designed for arc-second imaging in the submillimeter spectrum. SMA science spans an impressive array of fields, ranging from our solar system, through imaging of gas and dust and tracing magnetic fields in stellar nurser-ies and planet-forming disks, to exploration of nearby galaxies and imaging of dusty star-forming galaxies at high redshift. In addition to its outstanding record in astronomical research, the SMA is a world leader in the design of wide-bandwidth, high-frequency radio receivers for astronomy. The SMA recently commissioned a next generation correlator which vastly increases total bandwidth (to 8 GHz/sideband per polarization) while retaining high spectral resolution (140 kHz) across the entire processed spectral range, providing significantly enhanced science capability, and further expansion to 12 GHz/sideband per polarization is underway. These positions are aimed chiefly at research, both observational and theoretical, in submillimeter astronomy. Successful candidates will participate in remote and on-site observations with the SMA, research in their interpretation, and/or instrument development. While the SMA fellowships are intended primarily for research associated with the SMA, our main offices at the Center for Astrophysics provide Fellows with unique opportunities to develop collaborations within the wider CfA community and enjoy extraordinary free-dom in structuring their research activities. Applicants must have a recent Ph.D. in astronomy or a related field. The SMA received a total of 77 proposals (SAO 58) requesting observing time in the 2018A semester. The proposals received by the joint SAO and ASIAA Time Allocation Committee

Self-interacting dark matter offers an interesting alternative to collisionless dark matter because of its ability to preserve the large-scale success of the cold dark matter model, while seemingly solving its challenges on small scales. We present here the first study of the expected dark matter detection signal in a fully cosmological context taking into account different self-scattering models for dark matter. We demonstrate that models with constant and velocity-dependent cross-sections, which are consistent with observational constraints, lead to distinct signatures in the velocity distribution, because non-thermalized features found in the cold dark matter distribution are thermalized through particle scattering. Depending on the model, self-interaction can lead to a 10 per cent reduction of the recoil rates at high energies, corresponding to a minimum speed that can cause recoil larger than 300 km s(-1), compared to the cold dark matter case. At lower energies these differences are smaller than 5 per cent for all models. The amplitude of the annual modulation signal can increase by up to 25 per cent, and the day of maximum amplitude can shift by about two weeks with respect to the cold dark matter expectation. Furthermore, the exact day of phase reversal of the modulation signal can also differ by about a week between the different models. In general, models with velocity-dependent cross-sections peaking at the typical velocities of dwarf galaxies lead only to minor changes in the detection signals, whereas allowed constant cross-section models lead to significant changes. We conclude that different self-interacting dark matter scenarios might be distinguished from each other through the details of direct detection signals. Furthermore, detailed constraints on the intrinsic properties of dark matter based on null detections should take into account the possibility of self-scattering and the resulting effects on the detector signal.

We have investigated on the nature of the radio source near the star SAO206462. Although several recent efforts concluded that the galaxy does not significantly pollute the prominent IR flux of the star, we consider convenient to establish the properties of the galaxy and explore a method that can be used when a stellar FIR image is polluted by background extragalactic objects. Using archival data available from 2MASS, WISE and radio at 1.4 GHz, we conducted a comparison with the spectral energy distributions of a set of galaxy templates of different morphologies. Through a spectral energy distribution (SED) fitting method we have determined the galaxy photometric redshift, z(phot) similar to 0.1, its lR luminosity, L-IR 4x10(11)L(circle dot) and the star formation rate, 53M(circle dot)/yr. These properties, in addition to the possible presence of an obscured AGN, are consistent with the typical scenarios that characterize local luminous IR galaxies (LIRGs).

We derive an expression for the entropy of a present dark matter halo described by a Navarro-Frenk-White modified model with a central core. The comparison of this entropy with the one of the halo at the freeze-out era allows us to obtain an expression for the relic abundance of neutralinos, which in turn is used to constrain the parameter space in mSUGRA models, when used with the WMAP observations. Moreover, by joning these results with the ones obtained from the usual abundance criteria, we are able to clearly discriminate validity regions among tan beta values of the mSUGRA model, by demanding both criteria to be consistent with the 2 sigma bounds of the WMAP observations for the relic density: 0.112 < Omega h^2 < 0.122. We found that for sign mu positive, small values of tan beta are not favored; only for tan beta 50 are both criteria significantly consistent. The use of both criteria also allows us to put a lower bound on the neutralino mass of > 151 GeV.

We discuss the shape and decomposition of rotation curves (RCs) of galaxies formed within growing cold dark matter halos. The outer RC shape correlates mainly with the surface brightness (SB), the luminous mass fraction, f d , and the bulge fraction. In order the shapes of RC depend significantly on luminosity, f d should be a strong function of mass (feedback). For the preferred values of f d (< ∼ 0.03), the high SB models can be maximum disks only when the halos have a shallow core. The low SB models are sub-maximum disks. The residuals of the baryonic Tully-Fisher (TF) and mass-radius relations show a clear anti-correlation, but when one passes to the TF and L-R relations, the anti-correlation almost disappears. Therefore, the observed lack of correlation among the residuals of the last two relations should not be interpreted as an evidence of sub-maximal disks.

We discuss the shape and decomposition of rotation curves (RCs) of galaxies formed within growing cold dark matter (CDM) halos. The outer RC shapes correlates mainly with the surface brightness (SB), the luminous mass fraction, f(d), and the bulge fraction. In order that the shapes of RC depend significantly on luminosity, f(d) should be a strong function of mass (feedback). For the preferred values of f(d) (less than or similar to 0.03), the high SB models can only be maximum disks when the halos have a shallow core. The low SB models are sub-maximum disks. The residuals of the baryonic Tully-Fisher and mass-radius relations show a clear anti-correlation, but when one passes to the luminosity-amplitude of the RCs and the luminosity-radius relations, the anti-correlation almost disappears. Therefore, the observed lack of correlation among the residuals of the last two relations should not be interpreted as an evidence of sub-maximal disks.