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Binary statistics of the latest-type T and Y brown dwarfs are sparse and it is unclear whether the trends seen in the multiplicity properties of their more massive counterparts hold for the very coolest brown dwarfs. We present results from a search for substellar and planetary-mass companions to a sample of 12 ultracool T8$-$Y0 field brown dwarfs with the Hubble Space Telescope/Wide Field Camera 3. We find no evidence for resolved binary companions among our sample down to separations of 0.7$-$2.5 AU. Combining our survey with prior searches, we place some of the first statistically robust constraints to date on the multiplicity properties of the coolest, lowest-mass brown dwarfs in the field. Accounting for observational biases and incompleteness, we derive a binary frequency of $f = 5.5^{+5.2}_{-3.3}$% for T5$-$Y0 brown dwarfs at separations of 1.5$-$1000 AU, for an overall binary fraction of $f_\mathrm{tot} = 8\pm6$%. Modelling the projected separation as a lognormal distribution, we find a peak in separation at $\rho_0 = 2.9^{+0.8}_{-1.4}$ AU with a logarithmic width of $\sigma = 0.21^{+0.14}_{-0.08}$. We infer a mass ratio distribution peaking strongly towards unity, with a power law index of $\gamma = 6.1^{+4.0}_{-2.7}$, reinforcing the significance of the detection of a tighter and higher mass ratio companion population around lower-mass primaries. These results are consistent with prior studies and support the idea of a decreasing binary frequency with spectral type in the Galactic field.

We report the discovery of LEHPM 2-59 as the coolest extreme M subdwarf (esdM) found to date. Optical and near-infrared spectroscopy demonstrate that this source is of later spectral type than the esdM7 APMPM J0559 2903, with the presence of strong alkali lines (including Rb i), VO absorption at 7400 8, and H2O absorption at 1.4 m. Current optical classification schemes yield a spectral type of esdM8, making LEHPM 2-59 one of only two ultracool esdMs known. The substantial space velocity of this object (Vgalactic 180 km s1) identifies it as a halo star. Spectral model fits to the optical and near-infrared spectral data for this and four other late-type esdMs indicate that LEHPM 2-59 is the coolest esdM currently known, with TeA 2800 3000 K and 1:5P M/H P2:0. Comparison of TeA determinations for M dwarfs and esdMs based on spectral model fits from this study and the literature demonstrate a divergence in TeA scales beyond spectral typesM5/esdM5, as large as 600–800 K by types M8/esdM8. While this divergence is likely an artifact of the underlying classification scheme, it may lead to sys-tematic errors in the derived properties of intermediate metallicity subdwarfs. We comment on the future of ultracool subdwarf classification and suggest several ideas for addressing shortcomings in current (largely extrapolated) schemes.

We have used multi-epoch images from the Infrared Array Camera on board the Spitzer Space Telescope to search for substellar companions to stars in the solar neighborhood based on common proper motions. Through this work, we have discovered a faint companion to the white dwarf WD 0806-661. The comoving source has a projected separation of 130", corresponding to 2500 AU at the distance of the primary (19.2 pc). If it is physically associated, then its absolute magnitude at 4.5um is ~1 mag fainter than the faintest known T dwarfs, making it a strong candidate for the coolest known brown dwarf. The combination of M_4.5 and the age of the primary (1.5 Gyr) implies an effective temperature of ~300 K and a mass of ~7 M_Jup according to theoretical evolutionary models. The white dwarf's progenitor likely had a mass of ~2 M_sun, and thus could have been born with a circumstellar disk that was sufficiently massive to produce a companion with this mass. Therefore, the companion could be either a brown dwarf that formed like a binary star or a giant planet that was born within a disk and has been dynamically scattered to a larger orbit.

We have obtained a good quality R$\sim$400 0.8-2.5 $\mu$m spectrum and accurate photometry of Gl 570D, one of the coolest and least luminous brown dwarfs currently known. The spectrum shows that Gl 570D has deeper absorptions in the strong water and methane bands at 1.12-1.17 $\mu$m, 1.33-1.45 $\mu$m, 1.62-1.88 $\mu$m, and 2.20-2.45 $\mu$m and is both bluer at J-K and redder at $K-L^{\prime}$ than previously observed T dwarfs. Data analysis using model spectra coupled with knowledge of the well-understood primary implies that for the same surface gravity, Gl 570D is about 160 K cooler than Gl 229B. For an age range of 2-5 Gyr Gl 570D has an effective temperature in the range 784-824 K, a log gravity in the range 5.00-5.27 cm s$^{-2}$, and a luminosity in the range 2.88-2.98 $\times$ 10$^{-6}$ L$_\odot$.

We present the results of intense photometric monitoring in the near-infrared (~0.9 μm) with the TRAPPIST robotic telescope of the newly discovered binary brown dwarf WISE J104915.57-531906.1, the third closest system to the Sun at a distance of only 2 pc. Our twelve nights of time-series photometry reveal a quasi-periodic (P = 4.87 ± 0.01h) variability with a maximum peak-peak amplitude of ~11% and strong night-to-night evolution. We attribute this variability to the rotational modulation of fast-evolving weather patterns in the atmosphere of the coolest component (~T1-type) of the binary. No periodic signal is detected for the hottest component (~L8-type). For both brown dwarfs, our data allow us to firmly discard any unique transit during our observations for planets ≥2 R⊕. For orbital periods smaller than ~9.5 h, transiting planets are excluded down to an Earth-size.

We have obtained follow-up spectroscopy of eight late dwarf candidates discovered in a 105 deg2 area observed with the 2MASS Prototype Camera during test runs between 1992 and 1994. These objects were chosen because of their red infrared colors (e.g., J-Ks ≥ 1.10) and/or red OIR colors (e.g., R-Ks ≥ 6.00). All eight are late M dwarfs, six of which have spectral types later than van Biesbroeck 8 (type M7 V). Despite the fact that we have only followed up a fraction of the reddest sources discovered, the number of known M dwarfs of type M7 and cooler has been increased by 30%. Extrapolation of these results alone shows that over 2000 dwarfs of similar spectral type and with Ks ≤ 14.0 will be imaged by 2MASS over the entire sky. One of these new discoveries is astonishingly cool and has a tentative type of ≥M10 V. This dwarf, one of the least luminous objects yet discovered, could itself be a high-mass brown dwarf, thus providing another empirical data point in a regime where few such objects are now recognized. Only the substellar suspect GD 165 B and the bona fide brown dwarf GL 229 B, both discovered as companions to known stars, are cooler. Thus, this 2MASS discovery becomes the coolest isolated object so far identified.

Author: Sanders, J. S. et al.; Genre: Journal Article; Issued: 2013-03; Title: Velocity width measurements of the coolest X-ray emitting material in the cores of clusters, groups and elliptical galaxies

Understanding the processes that cause speciation is a key aim of evolutionary biology. Lineages or biomes that exhibit recent and rapid diversification are ideal model systems for determining these processes. Species rich biomes reported to be of relatively recent origin, i.e., since the beginning of the Miocene, include Mediterranean ecosystems such as the California Floristic Province, oceanic islands such as the Hawaiian archipelago and the Neotropical high elevation ecosystem of the Páramos. Páramos constitute grasslands above the forest tree-line (at elevations of c. 2800-4700 m) with high species endemism. Organisms that occupy this ecosystem are a likely product of unique adaptations to an extreme environment that evolved during the last three to five million years when the Andes reached an altitude that was capable of sustaining this type of vegetation. We compared net diversification rates of lineages in fast evolving biomes using 73 dated molecular phylogenies. Based on our sample, we demonstrate that average net diversification rates of Páramo plant lineages are faster than those of other reportedly fast evolving hotspots and that the faster evolving lineages are more likely to be found in Páramos than the other hotspots. Páramos therefore represent the ideal model system for studying diversification processes. Most of the speciation events that we observed in the Páramos (144 out of 177) occurred during the Pleistocene possibly due to the effects of species range contraction and expansion that may have resulted from the well-documented climatic changes during that period. Understanding these effects will assist with efforts to determine how future climatic changes will impact plant populations.

Cognitive Radio (CR) emerges as a promising solution to current unbalanced spectrum utilization. The cognitive ad hoc network can take advantage of dynamic spectrum access and spectrum diversity over wide spectrum. It could achieve higher network capacity compared to traditional ad hoc networks, thus supporting bandwidth-demanding applications. A cognitive radio operates over wide spectrum with unpredictable channel availability. Moreover, the transmission opportunity of a cognitive node is not guaranteed due to the presence of primary users (PUs). These two unique features define new routing problems in cognitive ad hoc networks. To better characterize the unique features of cognitive radio networks, we propose new routing metrics, including accumulated spectrum temperature, highest spectrum temperature, and mixed spectrum temperature to account for the time-varying spectrum availability. The proposed metrics favor the "coolest'' path, or the path with the most balanced and/or the lowest spectrum utilization by the primary users. We also study the computational complexity of the routing algorithm in cognitive ad hoc networks. Experiment results on our USRP-2 testbed show that the proposed metrics are capable of capturing the fluctuation of spectrum availability and suitable for cognitive ad hoc networks.

We present moderate resolution spectroscopy of 112 cool dwarf stars to supplement the observations we have already presented in the Palomar/MSU Nearby-Star Spectroscopic Survey. The sample consists of 72 suspected nearby stars added to the The Preliminary Third Catalog of Nearby Stars since 1991 as well as 40 faint red stars selected from the LHS catalog. LHS 1826 is more metal-poor and cooler than the coolest previously known extreme subdwarf, LHS 1742a. LHS 2195 is a very late M dwarf of type M8 V, probably at a distance of ten parsecs. LHS 1937 is an M7 V star at ∼ 20 parsecs. Three other previously unobserved LHS stars have estimated distances that place them within 25 parsecs. 1.

We report the discovery of seven high proper motion stars with proper motions between about 0.7 and 2.2 arcsec/yr, all at relatively low Galactic latitudes () and located in the southern sky. They were detected in a high proper motion search using multi-epoch positions in the optical SuperCOSMOS Sky Surveys and in the near-infrared sky surveys 2MASS and DENIS. Classification spectroscopy carried out for six of the objects reveals them to represent three different classes of cool objects in the solar neighbourhood: M dwarfs, M subdwarfs and cool white dwarfs. The star with the largest proper motion, SSSPM J1138–7722, is classified as a very nearby ( 8 pc) M 5.5 dwarf with Galactic thin disk kinematics. A second star with ~2 arcsec/yr proper motion, SSSPM J1358–3938, is still lacking spectroscopic confirmation but can be classified from photometry as a thick disk ~M 3.5 dwarf. Three objects turn out to be cool subdwarf members of the Galactic thick disk or halo, including the first sdM9.5 object, SSSPM J1013–1356, which represents the currently coolest known M subdwarf, another ultra-cool subdwarf, SSSPM J1930–4311, of spectral type sdM7.0 as well as an earlier type (sdM1.5) star. The latter, SSSPM J1530–8146, has an extremely large space velocity with clear halo kinematics (heliocentric km s-1). Two objects show featureless spectra classifying them as cool white dwarfs with K. One of them, SSSPM J1549–3544, is an extremely nearby ( pc) thin disk object, the other one, SSSPM J1148–7458, has thick disk kinematics. SSSPM J1549–3544 is likely to be the nearest cool white dwarf and may be even the nearest isolated white dwarf, i.e. closer than van Maanen 2.

Urbanization negatively impacts the urban environment mainly by the production of waste heat from refrigeration systems, although industrial processes and motorized vehicular traffic have also been recognized as additional causes of the urban heat island (UHI) effect. The UHI negatively impacts the residents, with spillover effects for environmental aspects. In urbanized areas, it is a critical factor for air quality management and public health. The UHI and strategies to implement its mitigation are becoming increasingly important for governmental agencies and researchers. The problem is how to deal with UHI effects? Accordingly, the main aim of this paper is to determine the UHI mitigation strategies and their effectiveness in terms of cooling and temperature reduction in cities at the level of urban design. This goal is achieved through exploring the concept of the cool city, as it is the key factor, from the theoretical, analytical, and practical viewpoints, to diminishing the urban heat release. Then, the paper analyzes how the concept of the coolest city in the world (Stuttgart, Germany) is developed and explores a practical approach toward cool cities. Finally, it suggests a set of recommendations to develop the urban environment in Greater Cairo by applying the cool city concept.

We explore the spectral and atmospheric properties of brown dwarfs cooler than the latest known T dwarfs. Our focus is on the yet-to-be-discovered free-floating brown dwarfs in the \\teff range from $\\sim$800 K to $\\sim$130 K and with masses from 25 to 1 \\mj. This study is in anticipation of the new characterization capabilities enabled by the launch of SIRTF and the eventual launch of JWST. We provide spectra from $\\sim$0.4 \\mic to 30 \\mic, highlight the evolution and mass dependence of the dominant H$_2$O, CH$_4$, and NH$_3$ molecular bands, consider the formation and effects of water-ice clouds, and compare our theoretical flux densities with the sensitivities of the instruments on board SIRTF and JWST. The latter can be used to determine the detection ranges from space of cool brown dwarfs. In the process, we determine the reversal point of the blueward trend in the near-infrared colors with decreasing \\teff, the \\teffs at which water and ammonia clouds appear, the strengths of gas-phase ammonia and methane bands, the masses and ages of the objects for which the neutral alkali metal lines are muted, and the increasing role as \\teff decreases of the mid-infrared fluxes longward of 4 \\mic. These changes suggest physical reasons to expect the emergence of at least one new stellar class beyond the T dwarfs. Our spectral models populate, with cooler brown dwarfs having progressively more planet-like features, the theoretical gap between the known T dwarfs and the known giant planets. Such objects likely inhabit the galaxy, but their numbers are as yet unknown.

The recycled pulsar PSR J2222–0137 is one of the closest known neutron stars (NSs) with a parallax distance of 267_(-0.9)^(+1.2) pc and an edge-on orbit. We measure the Shapiro delay in the system through pulsar timing with the Green Bank Telescope, deriving a low pulsar mass (1.20 ± 0.14 M_☉) and a high companion mass (1.05 ± 0.06 M_☉) consistent with either a low-mass NS or a high-mass white dwarf. We can largely reject the NS hypothesis on the basis of the system's extremely low eccentricity (3 × 10^(–4))—too low to have been the product of two supernovae under normal circumstances. However, despite deep optical and near-infrared searches with Southern Astrophysical Research and the Keck telescopes we have not discovered the optical counterpart of the system. This is consistent with the white dwarf hypothesis only if the effective temperature is <3000 K, a limit that is robust to distance, mass, and atmosphere uncertainties. This would make the companion to PSR J2222–0137 one of the coolest white dwarfs ever observed. For the implied age to be consistent with the age of the Milky Way requires the white dwarf to have already crystallized and entered the faster Debye-cooling regime.

Aims.We present an asteroseismological study of PG 0122+200, the coolest known pulsating PG 1159 (GW Vir) star. Our results are based on an augmented set of the full PG 1159 evolutionary models recently presented by Miller Bertolami & Althaus (2006).

The coolest dwarf stars targeted by the Kepler Mission constitute a relatively small but scientifically valuable subset of the Kepler target stars, and provide a high-fidelity, nearby sample of transiting planetary systems. Using archival Kepler data spanning the entire primary mission, we perform a uniform analysis to extract, confirm, and characterize the transit signals discovered by the Kepler pipeline toward M-type dwarf stars. We recover all but two of the signals reported in a recent listing from the Exoplanet Archive resulting in 163 planet candidates associated with a sample of 104 low-mass stars. We fitted the observed light curves to transit models using a Markov Chain Monte Carlo method and we have made the posterior samples publicly available to facilitate further studies. We fitted empirical transit times to individual transit signals with significantly non-linear ephemerides for accurate recovery of transit parameters and precise measuring of transit timing variations. We also provide the physical parameters for the stellar sample, including new measurements of stellar rotation, allowing the conversion of transit parameters into planet radii and orbital parameters.

Urban authorities and a range of private and civil society actors have come to view housing as a key arena in which to address climate change whilst also pursuing wider social, economic and environmental objectives. Housing has been a critical area for urban studies, but often considered in sectoral terms and work on urban responses to climate change has followed this positioning. By contrast, an Urban Political Ecology (UPE) perspective would position housing in more integrated terms as part of the metabolism of the city. Yet so far there has been relatively little written in UPE about either housing or climate change. This paper therefore seeks to bring UPE into dialogue with the emergent literature focused on governing climate change through housing. It does so through a detailed study of the ‘Retrofit Philly “Coolest Block” Contest’. We argue that this contest highlights the ways climate change is changing the way housing is embedded in the circulations of the city, pointing to changes in who is governing housing, how housing is being governed and who is able to access the benefits of (climate change-branded) action on housing.

We extend our previous study of the cool gas responsible for the emission of O vii X-ray lines in the cores of clusters and groups of galaxies. This is the coolest X-ray emitting phase and connects the 10 000 K H α emitting gas to the million degree phase, providing a useful tool to understand cooling in these objects. We study the location of the O vii gas and its connection to the intermediate Fe xvii and hotter O viii phases. We use high-resolution X-ray grating spectra of elliptical galaxies with strong Fe xvii line emission and detect O vii in 11 of 24 objects. Comparing the O vii detection level and resonant scattering, which is sensitive to turbulence and temperature, suggests that O vii is preferably found in cooler objects, where the Fe xvii resonant line is suppressed due to resonant scattering, indicating subsonic turbulence. Although a larger sample of sources and further observations is needed to distinguish between effects from temperature and turbulence, our results are consistent with cooling being suppressed at high turbulence as predicted by models of active galactic nuclei feedback, gas sloshing and galactic mergers. In some objects, the O vii resonant-to-forbidden line ratio is decreased by either resonant scattering or charge exchange boosting the forbidden line, as we show for NGC 4636. Charge exchange indicates interaction between neutral and ionized gas phases. The Perseus cluster also shows a high Fe xvii forbidden-to-resonance line ratio, which can be explained with resonant scattering by low-turbulence cool gas in the line of sight.