1107.1966
A new catalogue of polar-ring galaxies selected from the SDSS
Moiseev, Smirnova, Smirnova, Reshetnikov
* galaxies with polar rings?
Polar rings in galaxies can be used to study formation and evolution of galaxies, and study the properties of dark halos. Present new catalog of polar ring galaxies (PRGs) based on Galaxy Zoo. Previous: ~24, this catalog from SDSS: 70 galaxies as "best candidates", 115 good PRG candidates; 53 classified as PRG-related; 37 galaxies with their polar rings almost face-on. Sloan PRG's are on average fainter and located further away than the old (Whitmore-based) catalog (from 1990), but also includes nearby candidates. Spectroscopic observations of six galaxies: polar ring confirmed in 5, while the last one appeared to be a projection of two galaxies. Added 10 galaxies to the kinematically-confirmed PRGs.
* ooh, pretty pictures.
* ooh, pretty pictures.
1107.2067
Variability of the SiO thermal line emission toward the young L1448-mm outflow
Jiminez-Serra, Martin-Pintado, Winters, Rodriguez-Franco, Caselli
* C-shocks: no info
* what an awful first sentence of an abstract. I don't understand what's going on or what they're going to talk about. What outflow? Where?
* situation does not improve half-way through the abstract. What condensation?
Narrow SiO thermal emission towards young outflows has been proposed to be a signature of the magnetic precursor of C-shocks. Some study on some object. Something about a jet. Speculate something about the SiO features associated with the precursor of C-shocks appearing at the interface of the new SiO components seen at intermediate velocities.
* I still don't understand what the subject is about. Can't tell if this is about a star or a galaxy or what. And it's been accepted by ApJ. What a dorkus referee.
* first line of the intro: "Variability is a common phenomena in the evolution of very young stars." Aaaah, so we're talking about stars! Still not clear what a C-shock is. Dorks.
* I'm probably in a bad mood today.
1103.3505
Bias in low-multipole CMB reconstructions
Copi, Huterer, Schwarz, Starkman
Low l multipoles are hampered by cosmic variance and our Galaxy. Reconstruction of full sky from partial sky is biased due to leakage of info from obscured region to the used region. Using the unobscured region without reconstructing is the most robust way to measure the true CMB sky. For noise-free data, the usual optimal, unbiased estimator can be employed without smoothing, avoiding the leakage problem. But real data with noise and residual foregrounds yields highly biased reconstructions.
1107.0682
Violation of the rotational invariance in the CMB bispectrum
Shiraishi, Yokoyama
* I've read this one before, it's about some theoretical cr.. stuff.
quantum fluctuations of a vector field can imprint on CMB as rotational invariance in the CMB bispectrum.
1107.2920
Starspots, spin-orbit misalignment, and active latitudes in the HAT-P-11 exoplanetary system
Sanchis-Ojeda, Winn
* Rossiter-McLaughlin effect: a spectroscopic phenomenon observed when an eclipsing binary's exoplanet/secondary star transits across the face of the parent/primary star.
Observed 26 transits of super-Neptune exoplanet, where they also expect starspots rotating at the "active latitude", causing some anomaly when the planet transits across the spots. Rossiter-McLaughlin effect also observed, find two solutions for the stellar obliquity (psi) and active latitude (l). Future observations should reveal changes in the preferred phases of spot-crossing anomalies.
1107.3120
AzTEC 1.1 mm images of 16 radio galaxies at 0.5<z<5.2 and a quasar at z=6.3
Humphrey et al
Observed 16 radio galaxies at high z + a radio-quiet quasar at z=6.3 at 1.1mm, more than doubling the number of high-z radio galaxies imaged at millimeter/sub-millimeter wavelengths. 11 of the active galaxies show mm counterpart signals (probably). The other 6 have one more more likely associated mm source. Thus, powerful radio-loud galaxies at high-z are beacons for finding luminous mm/sub-mm galaxies at high-z.
Combine with Spitzer, examine the mid-infrared colors of sample. Those with 1.1 mm counterpart are consistent with dusty starbursts, and are bluer than high-z Spitzer-selected active galaxes. Additionally, find arcs of 200-500 kpc apparently associated with 3 of the radio galaxies.
1107.3137
An HST/WFC3-IR morphological survey of galaxies at z=1.5-3.6: I. Survey description and morphological properties of star forming galaxies
Law, Steidel, Shapley, Nagy, Reddy, Erb
Study rest-frame optical morphologies of star-forming galaxies at z=1.5-3.6 with HST. 42 orbits, F160W (why in blue?), 65 arcmin^2, 27.9 AB mag (5 sigma, 0.2" radius aperture). M* ranges from 1e9 to 1e11 M_sun, 306 SF galaxies, half-light radii range of 0.7-3.0kpc. A stellar mass-radius relation described at z~3. Distribution of axis rations strongly inconsistent with a population of inclined exponential disks--better reproduced by triaxial stellar systems with c/a and b/a ratio of 0.3 and 0.7, respectively. Rest-UV and Rest-optical morphologies are generally similar for subset of HST imaging data; differences are pronounced at higher masses of M* > 3e10 M_sun. Gas-phase kinematics related to morphological maturity of the system and degree of rotational support; larger galaxies and more disk-like kinematics have a large quantity of gas at the systemic redshift that produces interstellar absorption lines whose centroids are systematically less blueshifted than in their smaller-dispersion counterparts. (what?) Discuss galaxy morphology in the context of merger fraction constraints: morphologically-identified mergers/non-mergers generally have insignificant differences in terms of physical observables such as stellar mass, SFR, and gas-phase kinematics.
* I guess I don't really understand what they mean when they say "gas-phase kinematics".
* And that sentence about gas-phase kinematics and morphological maturity is confusing as hell. I still don't get what they're trying to say.
0903.2732
F(R) cosmology in presence of a phantom fluid and its scalar-tensor counterpart: towards a unified precision model of the universe evolution
Elizalde, Saez-Gomez
Phantom fluid introduced in an f(R) model. Dark fluid gives rise to deceleration in early universe; today they add to the effective cosmological constant; later, produces transition toa "phantom era" (whoa) which may already have observable consequences. Dark fluid dominates at Rip time. Dark fluid with phantom behavior gives rise to super-accelerated phase. F(R) model can be constructed from a phantom model in a scalar-tensor theory.
* what are the observable consequences? That should be in the abstract.
1102.5363
The effect of helium sedimentation on galaxy cluster masses and scaling relations
Bulbul, Hasler, Bonamente, Joy, Marrone, Miller, Mroczkowski
Inner regions of galaxy clusters may have an enhanced He abundance due to sedimentation, which may affect the cluster mass estimates. Chandra observation of 8 relaxed galaxy clusters, investigate upper limits to the effect of He sedimentation to the relation Y_X vs M_500 and Y_X-M_2500. Calculate gas mass and total mass in two limits: un-enhanced abundance distribution and radial distribution of He sedimentation over 11 Gyrs. The sedimentation model produces a negligible increase in the gas mass within r<r500 (1.3%) and a 10% decrease in the total mass w/in r<r500. Stronger effect at smaller radii due to larger variance in He abundance in the inner region. Slope of the Y_X-M500 scaling relation is not significantly affected with He sedimentation.
* if He sedimentation is true, then mass estimates of M500 can be off by up to +10%, but the Y_X-M500 relation slope doesn't change much.
1107.2564
Testing the WMAP cosmology via Planck radio catalogues
Whitbourn, Shankes, Sawangwit
* I read this one before
Beam profile affects CMB experiments, but some discrepancies in WMAP and Planck observed in galaxy cluster SZ effects can't seem to be fixed.
1107.3160
Astroinformatics of galaxies and quasars: a new general method for photometric redshifts estimation
Laurino, D'Abrusco, Longo, Riccio
Weak Gated Experts (WGE) method: combination of data mining techiniques to determine photo-z. Sigma of 0.02 in (presumably the MAIN) galaxy; WGE also provides accuracy estimates. Works for quasars too.
* I still believe in the scientifically-based method of template fitting, not "informatics".
1106.3182
Enhanced sensitivity to dark matter self-annihilations in the sun using Neurtrino Spectral information
Rott, Tanaka, Itow
Self-annihilating DM particles captured gravitationally in the sun can generate observable neutrino signals. Detect spin-dependent scattering of WIMPs with nucleons in the Sun. Describe how to convert neutrino fluxes to WIMP-nucleon cross section (how?). Sensitive to low mass WIMPs; best results obtained with e- neutrino channel.
* how?
1107.3131
Requiem for an FCHAMP?
Langacker, Steigman
* whoa, Langacker!
FCHAMP: fractionally charged massive particles; appear in extension of the std model with superstring constructions. Lightest FCHAMP should be in existence today due to its stability. Massively charged particles behave like baryons, affects primordial nucleosynthesis and CMB anisotropies; measurements limit the FCHAMP relic density. Accelerator searches also constrain. FCHAMP can combine with alpha particles and protons, forming a tighly bound, positively charged states. ... I lost interest in this abstract.
* Do they mean electrical charge? In which case, I think the photons can see it (it's observable, not a dark form of matter)?
1107.2934
The baryonic Tully-Fisher relation of gas rich galaxies as a test of LCDM and MOND
McGaugh
Baryonic Tully-Fisher relation (BTFR): empirical realtion between garyonic mass and rotation velocity in disk galaxies; can test LCDM galaxy formation models, and MOND. Uses gas mass instead of stellar mass. ... galaxies that have experiences the least star formation have been most impacted by feedback.
* am I getting lazy, or are these abstracts not interesting?
1107.2944
Renegade subhaloes in the local group
Knebe, Libeskind, Doumler, Yepes, Cottloeber, Hoffman
Renegade subhalos: subhaloes that change their affiliation from one of the two prominent hosts to the other (e.g., from Milky way to Andromeda; LMC and SMC spawed near Andromeda?). N-body simulation suggest that the renegade subhaloes appear to be flying past one host before being pulled into the other. Merger not required to trigger such an event. Simulated Local Group facilitate such behavior. Small fraction of the full z=0 subhalo populations are renegades--intrinsically difficult to distinguish them despite clear differences in velocity, radial distribution, shape and spin-parameter distributions.
* first line of the intro: "Variability is a common phenomena in the evolution of very young stars." Aaaah, so we're talking about stars! Still not clear what a C-shock is. Dorks.
* I'm probably in a bad mood today.
1103.3505
Bias in low-multipole CMB reconstructions
Copi, Huterer, Schwarz, Starkman
Low l multipoles are hampered by cosmic variance and our Galaxy. Reconstruction of full sky from partial sky is biased due to leakage of info from obscured region to the used region. Using the unobscured region without reconstructing is the most robust way to measure the true CMB sky. For noise-free data, the usual optimal, unbiased estimator can be employed without smoothing, avoiding the leakage problem. But real data with noise and residual foregrounds yields highly biased reconstructions.
1107.0682
Violation of the rotational invariance in the CMB bispectrum
Shiraishi, Yokoyama
* I've read this one before, it's about some theoretical cr.. stuff.
quantum fluctuations of a vector field can imprint on CMB as rotational invariance in the CMB bispectrum.
1107.2920
Starspots, spin-orbit misalignment, and active latitudes in the HAT-P-11 exoplanetary system
Sanchis-Ojeda, Winn
* Rossiter-McLaughlin effect: a spectroscopic phenomenon observed when an eclipsing binary's exoplanet/secondary star transits across the face of the parent/primary star.
Observed 26 transits of super-Neptune exoplanet, where they also expect starspots rotating at the "active latitude", causing some anomaly when the planet transits across the spots. Rossiter-McLaughlin effect also observed, find two solutions for the stellar obliquity (psi) and active latitude (l). Future observations should reveal changes in the preferred phases of spot-crossing anomalies.
1107.3120
AzTEC 1.1 mm images of 16 radio galaxies at 0.5<z<5.2 and a quasar at z=6.3
Humphrey et al
Observed 16 radio galaxies at high z + a radio-quiet quasar at z=6.3 at 1.1mm, more than doubling the number of high-z radio galaxies imaged at millimeter/sub-millimeter wavelengths. 11 of the active galaxies show mm counterpart signals (probably). The other 6 have one more more likely associated mm source. Thus, powerful radio-loud galaxies at high-z are beacons for finding luminous mm/sub-mm galaxies at high-z.
Combine with Spitzer, examine the mid-infrared colors of sample. Those with 1.1 mm counterpart are consistent with dusty starbursts, and are bluer than high-z Spitzer-selected active galaxes. Additionally, find arcs of 200-500 kpc apparently associated with 3 of the radio galaxies.
1107.3137
An HST/WFC3-IR morphological survey of galaxies at z=1.5-3.6: I. Survey description and morphological properties of star forming galaxies
Law, Steidel, Shapley, Nagy, Reddy, Erb
Study rest-frame optical morphologies of star-forming galaxies at z=1.5-3.6 with HST. 42 orbits, F160W (why in blue?), 65 arcmin^2, 27.9 AB mag (5 sigma, 0.2" radius aperture). M* ranges from 1e9 to 1e11 M_sun, 306 SF galaxies, half-light radii range of 0.7-3.0kpc. A stellar mass-radius relation described at z~3. Distribution of axis rations strongly inconsistent with a population of inclined exponential disks--better reproduced by triaxial stellar systems with c/a and b/a ratio of 0.3 and 0.7, respectively. Rest-UV and Rest-optical morphologies are generally similar for subset of HST imaging data; differences are pronounced at higher masses of M* > 3e10 M_sun. Gas-phase kinematics related to morphological maturity of the system and degree of rotational support; larger galaxies and more disk-like kinematics have a large quantity of gas at the systemic redshift that produces interstellar absorption lines whose centroids are systematically less blueshifted than in their smaller-dispersion counterparts. (what?) Discuss galaxy morphology in the context of merger fraction constraints: morphologically-identified mergers/non-mergers generally have insignificant differences in terms of physical observables such as stellar mass, SFR, and gas-phase kinematics.
* I guess I don't really understand what they mean when they say "gas-phase kinematics".
* And that sentence about gas-phase kinematics and morphological maturity is confusing as hell. I still don't get what they're trying to say.
0903.2732
F(R) cosmology in presence of a phantom fluid and its scalar-tensor counterpart: towards a unified precision model of the universe evolution
Elizalde, Saez-Gomez
Phantom fluid introduced in an f(R) model. Dark fluid gives rise to deceleration in early universe; today they add to the effective cosmological constant; later, produces transition toa "phantom era" (whoa) which may already have observable consequences. Dark fluid dominates at Rip time. Dark fluid with phantom behavior gives rise to super-accelerated phase. F(R) model can be constructed from a phantom model in a scalar-tensor theory.
* what are the observable consequences? That should be in the abstract.
1102.5363
The effect of helium sedimentation on galaxy cluster masses and scaling relations
Bulbul, Hasler, Bonamente, Joy, Marrone, Miller, Mroczkowski
Inner regions of galaxy clusters may have an enhanced He abundance due to sedimentation, which may affect the cluster mass estimates. Chandra observation of 8 relaxed galaxy clusters, investigate upper limits to the effect of He sedimentation to the relation Y_X vs M_500 and Y_X-M_2500. Calculate gas mass and total mass in two limits: un-enhanced abundance distribution and radial distribution of He sedimentation over 11 Gyrs. The sedimentation model produces a negligible increase in the gas mass within r<r500 (1.3%) and a 10% decrease in the total mass w/in r<r500. Stronger effect at smaller radii due to larger variance in He abundance in the inner region. Slope of the Y_X-M500 scaling relation is not significantly affected with He sedimentation.
* if He sedimentation is true, then mass estimates of M500 can be off by up to +10%, but the Y_X-M500 relation slope doesn't change much.
1107.2564
Testing the WMAP cosmology via Planck radio catalogues
Whitbourn, Shankes, Sawangwit
* I read this one before
Beam profile affects CMB experiments, but some discrepancies in WMAP and Planck observed in galaxy cluster SZ effects can't seem to be fixed.
1107.3160
Astroinformatics of galaxies and quasars: a new general method for photometric redshifts estimation
Laurino, D'Abrusco, Longo, Riccio
Weak Gated Experts (WGE) method: combination of data mining techiniques to determine photo-z. Sigma of 0.02 in (presumably the MAIN) galaxy; WGE also provides accuracy estimates. Works for quasars too.
* I still believe in the scientifically-based method of template fitting, not "informatics".
1106.3182
Enhanced sensitivity to dark matter self-annihilations in the sun using Neurtrino Spectral information
Rott, Tanaka, Itow
Self-annihilating DM particles captured gravitationally in the sun can generate observable neutrino signals. Detect spin-dependent scattering of WIMPs with nucleons in the Sun. Describe how to convert neutrino fluxes to WIMP-nucleon cross section (how?). Sensitive to low mass WIMPs; best results obtained with e- neutrino channel.
* how?
1107.3131
Requiem for an FCHAMP?
Langacker, Steigman
* whoa, Langacker!
FCHAMP: fractionally charged massive particles; appear in extension of the std model with superstring constructions. Lightest FCHAMP should be in existence today due to its stability. Massively charged particles behave like baryons, affects primordial nucleosynthesis and CMB anisotropies; measurements limit the FCHAMP relic density. Accelerator searches also constrain. FCHAMP can combine with alpha particles and protons, forming a tighly bound, positively charged states. ... I lost interest in this abstract.
* Do they mean electrical charge? In which case, I think the photons can see it (it's observable, not a dark form of matter)?
1107.2934
The baryonic Tully-Fisher relation of gas rich galaxies as a test of LCDM and MOND
McGaugh
Baryonic Tully-Fisher relation (BTFR): empirical realtion between garyonic mass and rotation velocity in disk galaxies; can test LCDM galaxy formation models, and MOND. Uses gas mass instead of stellar mass. ... galaxies that have experiences the least star formation have been most impacted by feedback.
* am I getting lazy, or are these abstracts not interesting?
1107.2944
Renegade subhaloes in the local group
Knebe, Libeskind, Doumler, Yepes, Cottloeber, Hoffman
Renegade subhalos: subhaloes that change their affiliation from one of the two prominent hosts to the other (e.g., from Milky way to Andromeda; LMC and SMC spawed near Andromeda?). N-body simulation suggest that the renegade subhaloes appear to be flying past one host before being pulled into the other. Merger not required to trigger such an event. Simulated Local Group facilitate such behavior. Small fraction of the full z=0 subhalo populations are renegades--intrinsically difficult to distinguish them despite clear differences in velocity, radial distribution, shape and spin-parameter distributions.
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