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The TOI-1130 is a known planetary system around a K-dwarf consisting of a gas giant planet, TOI-1130 c, on an 8.4-day orbit, accompanied by an inner Neptune-sized planet, TOI-1130 b, with an orbital period of 4.1 days. We collected precise radial velocity (RV) measurements of TOI-1130 with the HARPS and PFS spectrographs as part of our ongoing RV follow-up program. We perform a photodynamical modeling of the HARPS and PFS RVs, and transit photometry from the Transiting Exoplanet Survey Satellite (TESS) and the TESS Follow-up Observing Program. We determine the planet masses and radii of TOI-1130 b and TOI-1130 c to be Mb = 19.28 $\pm$ 0.97 M$_\oplus$ and Rb = 3.56 $\pm$ 0.13 R$_\oplus$, and Mc = 325.59 $\pm$ 5.59 M$_\oplus$ and Rc = 13.32+1.55-1.41 R$_\oplus$, respectively. We spectroscopically confirm TOI-1130 b that was previously only validated. We find that the two planets orbit with small eccentricities in a 2:1 resonant configuration. This is the first known system with a hot Jupiter and an inner lower mass planet locked in a mean-motion resonance. TOI-1130 belongs to the small yet increasing population of hot Jupiters with an inner low-mass planet that challenges the pathway for hot Jupiter formation. We also detect a linear RV trend possibly due to the presence of an outer massive companion., Comment: 19 pages, Accepted to A&A

The main scientific goal of TESS is to find planets smaller than Neptune around stars bright enough to allow further characterization studies. Given our current instrumentation and detection biases, M dwarfs are prime targets to search for small planets that are in (or nearby) the habitable zone of their host star. Here we use photometric observations and CARMENES radial velocity measurements to validate a pair of transiting planet candidates found by TESS. The data was fitted simultaneously using a Bayesian MCMC procedure taking into account the stellar variability present in the photometric and spectroscopic time series. We confirm the planetary origin of the two transiting candidates orbiting around TOI-2095 (TIC 235678745). The star is a nearby M dwarf ($d = 41.90 \pm 0.03$ pc, $T_{\rm eff} = 3759 \pm 87$ K, $V = 12.6$ mag) with a stellar mass and radius of $M_\star = 0.44 \pm 0.02 \; M_\odot$ and $R_\star = 0.44 \pm 0.02 \; R_\odot$, respectively. The planetary system is composed of two transiting planets: TOI-2095b with an orbital period of $P_b = 17.66484 \pm (7\times 10^{-5})$ days and TOI-2095c with $P_c = 28.17232 \pm (14\times 10^{-5})$ days. Both planets have similar sizes with $R_b = 1.25 \pm 0.07 \; R_\oplus$ and $R_c = 1.33 \pm 0.08 \; R_\oplus$ for planet b and c, respectively. We put upper limits on the masses of these objects with $M_b < 4.1 \; M_\oplus$ for the inner and $M_c < 7.4 \; M_\oplus$ for the outer planet (95\% confidence level). These two planets present equilibrium temperatures in the range of 300 - 350 K and are close to the inner edge of the habitable zone of their star., Submitted to Astronomy & Astrophysics

We report the discovery by the TESS mission of a super-Earth on a 4.8-d orbit around an inactive M4.5 dwarf (TOI-1680) validated by ground-based facilities. The host star is located 37.14 pc away, with a radius of 0.2100+/-0.0064 R_sun, mass of 0.1800+/-0.0044 M_sun and an effective temperature of 3211+/-100 K. We validated and characterized the planet using TESS data, ground-based multi-wavelength photometry from TRAPPIST, SPECULOOS, and LCO, as well as high-resolution AO observations from Keck/NIRC2 and Shane. Our analyses have determined the following parameters for the planet: a radius of 1.466+0.063/-0.049 R_earth and an equilibrium temperature of 404+/-14 K, assuming no albedo and perfect heat redistribution. Assuming a mass based on mass-radius relations, this planet is a promising target for atmospheric characterization with the James Webb Space Telescope (JWST)., Comment: Accepted in A&A

We present the discovery and validation of two TESS exoplanets orbiting nearby M dwarfs: TOI-2084b, and TOI-4184b. We characterized the host stars by combining spectra from Shane/Kast and Magellan/FIRE, SED (Spectral Energy Distribution) analysis, and stellar evolutionary models. In addition, we used Gemini-South/Zorro & -North/Alopeke high-resolution imaging, archival science images, and statistical validation packages to support the planetary interpretation. We performed a global analysis of multi-colour photometric data from TESS and ground-based facilities in order to derive the stellar and planetary physical parameters for each system. We find that TOI-2084b and TOI-4184b are sub-Neptune-sized planets with radii of Rp = 2.47 +/- 0.13R_Earth and Rp = 2.43 +/- 0.21R_Earth, respectively. TOI-2084b completes an orbit around its host star every 6.08 days, has an equilibrium temperature of T_eq = 527 +/- 8K and an irradiation of S_p = 12.8 +/- 0.8 S_Earth. Its host star is a dwarf of spectral M2.0 +/- 0.5 at a distance of 114pc with an effective temperature of T_eff = 3550 +/- 50 K, and has a wide, co-moving M8 companion at a projected separation of 1400 au. TOI-4184b orbits around an M5.0 +/- 0.5 type dwarf star (Kmag = 11.87) each 4.9 days, and has an equilibrium temperature of T_eq = 412 +/- 8 K and an irradiation of S_p = 4.8 +/- 0.4 S_Earth. TOI-4184 is a metal poor star ([Fe/H] = -0.27 +/- 0.09 dex) at a distance of 69 pc with an effective temperature of T_eff = 3225 +/- 75 K. Both planets are located at the edge of the sub-Jovian desert in the radius-period plane. The combination of the small size and the large infrared brightness of their host stars make these new planets promising targets for future atmospheric exploration with JWST., Accepted for publication in A&A

Context. Exoplanets with orbital periods of less than one day are known as ultra-short period (USP) planets. They are relatively rare products of planetary formation and evolution processes, but especially favourable for characterisation with current planet detection methods. At the time of writing, 125 USP planets have already been confirmed. Aims. Our aim is to validate the planetary nature of two new transiting planet candidates around M dwarfs announced by the NASA Transiting Exoplanet Survey Satellite (TESS), registered as TESS Objects of Interest (TOIs) TOI-1442.01 and TOI-2445.01. Methods. We used TESS data, ground-based photometric light curves, and Subaru/IRD spectrograph radial velocity (RV) measurements to validate both planetary candidates and to establish their physical properties. Results. TOI-1442 b is a validated exoplanet with an orbital period of $P$=0.4090682+/-0.0000004 d, a radius of $R_p$=1.15+/-0.06$R_{\oplus}$, and equilibrium temperature of $T_{p,eq}$=1357$_{-42}^{+49}$K. TOI-2445 b is also validated with an orbital period of $P$=0.3711286+/-0.0000004 d, a radius of $R_p$= 1.33+/-0.09$R_{\oplus}$, and equilibrium temperature of $T_{p,eq}$=1330$_{-56}^{+61}$K. Their physical properties align with current empirical trends and formation theories of USP planets. Based on the RV measurements, we set 3$\sigma$ upper mass limits of 8$M_{\oplus}$ and 20$M_{\oplus}$, thus confirming the non-stellar, sub-Jovian nature of both transiting objects. More RV measurements will be needed to constrain the planetary masses and mean densities, and the predicted presence of outer planetary companions. These targets extend the small sample of USP planets orbiting around M dwarfs up to 21 members. They are also among the 20 most suitable terrestrial planets for atmospheric characterisation via secondary eclipse with the JWST, according to a widespread emission spectroscopy metric., Comment: Published in A&A, 18 pages, 6 tables, 8 figures

We characterize Galactic dust filaments by correlating BICEP/Keck and Planck data with polarization templates based on neutral hydrogen (H I) observations. Dust polarization is important for both our understanding of astrophysical processes in the interstellar medium (ISM) and the search for primordial gravitational waves in the cosmic microwave background (CMB). In the diffuse ISM, H I is strongly correlated with the dust and partly organized into filaments that are aligned with the local magnetic field. We analyze the deep BICEP/Keck data at 95, 150, and 220 GHz, over the low-column-density region of sky where BICEP/Keck has set the best limits on primordial gravitational waves. We separate the H I emission into distinct velocity components and detect dust polarization correlated with the local Galactic H I but not with the H I associated with Magellanic Stream I. We present a robust, multifrequency detection of polarized dust emission correlated with the filamentary H I morphology template down to 95 GHz. For assessing its utility for foreground cleaning, we report that the H I morphology template correlates in B modes at a $\sim$10-65$\%$ level over the multipole range $20 < \ell < 200$ with the BICEP/Keck maps, which contain contributions from dust, CMB, and noise components. We measure the spectral index of the filamentary dust component spectral energy distribution to be $β= 1.54 \pm 0.13$. We find no evidence for decorrelation in this region between the filaments and the rest of the dust field or from the inclusion of dust associated with the intermediate velocity H I. Finally, we explore the morphological parameter space in the H I-based filamentary model., 27 pages, 12 figures

H. P. Osborn et al., [Context] TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young (340 ± 80 Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each., [Aims] To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements., [Methods] We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes., [Results] CHEOPS observations revealed a clear detection for TOI-2076 c at d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the P = 35.12537 ± 0.00067 d alias. These observations also improved the radius precision of all three sub-Neptunes to 2.518 ± 0.036, 3.497 ± 0.043, and 3.232 ± 0.063 R⊕. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST., CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. This material is based upon work supported by the National Science Foundation through the US Community Open Access to LCO facilities provided under Grant No. 2034337. This paper is based on observations made with the MuSCAT3 instrument, developed by Astrobiology Center and under financial supports by JSPS KAKENHI (JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. This research made use of exoplanet (Foreman-Mackey et al. 2021a,b) and its dependencies (Agol et al. 2020; Kumar et al. 2019; Astropy Collaboration 2013, 2018; Kipping 2013; Luger et al. 2019; Salvatier et al. 2016; Theano Development Team 2016). This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. AT acknowledges support from an STFC PhD studentship. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. DG and LMS gratefully acknowledge financial support from the Cassa di Risparmio di Torino (CRT) foundation under Grant No. 2018.2323 “Gaseousor rocky? Unveiling the nature of small worlds”. SGS acknowledges the support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). This work was supported by FCT – Fundacçâo para a Ciência e Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalizaçâo by these grants: PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FISAST/28987/2017 and POCI-01-0145-FEDER-028987. ACC and TGW acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1. VVG is a FRS-FNRS Research Associate. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. LBo, GPi, VNa, GSs, IPa, and RRa acknowledge the funding support from Italian Space Agency (ASI) regulated by “Accordo ASI-INAF n. 2013-016-R.O del 9 luglio 2013 e integrazione del 9 luglio 2015 CHEOPS Fasi A/B/C”. MIH and YA acknowledge the support of the Swiss National Fund under grant 200020_172746. ML acknowledges support of the Swiss National Science Foundation under grant number PCEFP2J94576. ABr was supported by the SNSA. B-OD acknowledges support from the Swiss National Science Foundation (PP00P2-190080). PM acknowledges support from STFC research grant number ST/M001040/1. This work is partly financed by the Spanish Mnistry of Economics and Competitiveness through grants PGC2018-098153-B-C31 Acknowledges support from the Spanish Mnistry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B-C33, as well as the support of the Generalitat de Catalunya/CERCA programme. This project was supported by the CNES MG is an FRS-FNRS Senior Research Associate. GyMSz acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a a PRODEX Experiment Agreement No. 4000137122, the Lendület LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements dAvenir supervised by the Agence Nationale pour la Recherche LD is an FRS-FNRS Postdoctoral Researcher. MF gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). This work was supported by FCT - Fundaçâo para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalizaçâo by these grants: UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113, PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987, ODSD is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. We acknowledge support from the Spanish Mnistry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia Maria de Maeztu-Centro de Astrobiología (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. XB, SC, DG, MF and JL acknowledge their role as ESA-appointed CHEOPS science team members. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement no. 724427); DE acknowledges financial support from the Swiss National Science Foundation for project 200021_200726. (covered by Tom Wilson’s acknowledgement) This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). SH gratefully acknowledges CNES funding through the grant 837319. KGI is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. YGMC is supported by UNAM-PAPIIT-IG101321. This work includes observations with SAINT-EX carried out at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir (OAN-SPM), Baja California, México. SS have received funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (grant agreement no. 833925, project STAREX).

We present an improved search for axion-like polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. An all-sky, temporally sinusoidal rotation of CMB polarization, equivalent to a time-variable cosmic birefringence, is an observable manifestation of a local axion field and potentially allows a CMB polarimeter to detect axion-like dark matter directly. We describe improvements to the method presented in previous work, and we demonstrate the updated method with an expanded dataset consisting of the 2012-2015 observing seasons. We set limits on the axion-photon coupling constant for mass $m$ in the range $10^{-23}$-$10^{-18}~\mathrm{eV}$, which corresponds to oscillation periods on the order of hours to years. Our results are consistent with the background model. For periods between $1$ and $30~\mathrm{d}$ ($1.6 \times 10^{-21} \leq m \leq 4.8 \times 10^{-20}~\mathrm{eV}$), the $95\%$-confidence upper limits on rotation amplitude are approximately constant with a median of $0.27^\circ$, which constrains the axion-photon coupling constant to $g_{\phi\gamma} < (4.5 \times 10^{-12}~\mathrm{GeV}^{-1}) m/(10^{-21}~\mathrm{eV}$), if axion-like particles constitute all of the dark matter. More than half of the collected BICEP dataset has yet to be analyzed, and several current and future CMB polarimetry experiments can apply the methods presented here to achieve comparable or superior constraints. In the coming years, oscillation measurements can achieve the sensitivity to rule out unexplored regions of the axion parameter space., Comment: 14 pages, 3 figures

We report on a series of 42 measurements of the transition frequency of the 429~THz (5s$^2$)~$^1$S$_0$--(5s5p)~$^3$P$_0$ line in $^{87}$Sr taken over three years from 2017 to 2019. They have been performed at the Physikalisch-Technische Bundesanstalt (PTB) between the laboratory strontium lattice clock and the primary caesium fountain clocks CSF1 and CSF2. The length of each individual measurement run has been extended by use of a hydrogen maser as flywheel to improve the statistical uncertainty given by the Cs clocks. We determine an averaged transition frequency of $429\:228\:004\:229\:873.00(0.07)$~Hz with $1.5\times10^{-16}$ fractional uncertainty, at the limit of the current realization of the unit hertz. Analysis of the data provides an improved limit on the coupling of the gravitational potential of the Sun to the proton--electron mass ratio $\mu$, and confirms the limits on its temporal drift., Comment: 8 pages, 4 figures

Let $A=(a_1,\ldots,a_n)$ be a vector of integers with $d=\sum_{i=1}^n a_i$. By partial resolution of the classical Abel-Jacobi map, we construct a universal twisted double ramification cycle $\mathsf{DR}^{\mathsf{op}}_{g,A}$ as an operational Chow class on the Picard stack $\mathfrak{Pic}_{g,n,d}$ of $n$-pointed genus $g$ curves carrying a degree $d$ line bundle. The method of construction follows the log (and b-Chow) approach to the standard double ramification cycle with canonical twists on the moduli space of curves [arXiv:1707.02261, arXiv:1711.10341, arXiv:1708.04471]. Our main result is a calculation of $\mathsf{DR}^{\mathsf{op}}_{g,A}$ on the Picard stack $\mathfrak{Pic}_{g,n,d}$ via an appropriate interpretation of Pixton's formula in the tautological ring. The basic new tool used in the proof is the theory of double ramification cycles for target varieties [arXiv:1812.10136]. The formula on the Picard stack is obtained from [arXiv:1812.10136] for target varieties $\mathbb{CP}^n$ in the limit $n \rightarrow \infty$. The result may be viewed as a universal calculation in Abel-Jacobi theory. As a consequence of the calculation of $\mathsf{DR}^{\mathsf{op}}_{g,A}$ on the Picard stack $\mathfrak{Pic}_{g,n,d}$, we prove that the fundamental classes of the moduli spaces of twisted meromorphic differentials in $\overline{\mathcal{M}}_{g,n}$ are exactly given by Pixton's formula (as conjectured in the appendix to [arXiv:1508.07940] and in [arXiv:1607.08429]). The comparison result of fundamental classes proven in [arXiv:1909.11981] plays a crucial role in our argument. We also prove the set of relations in the tautological ring of the Picard stack $\mathfrak{Pic}_{g,n,d}$ associated to Pixton's formula., Comment: 122 pages. v2: This is the Author Accepted Manuscript, to appear in Acta Mathematica (open access). Main change since v1 is addition of Section 6.2 discussing a refinement of the definition (due to Marcus and Wise) of logarithmic rubber maps. Comments still very welcome

We present results from an analysis of all data taken by the bicep2/Keck CMB polarization experiments up to and including the 2015 observing season. This includes the first Keck Array observations at 220 GHz and additional observations at 95 and 150 GHz. The Q and U maps reach depths of 5.2, 2.9, and 26 μK_{CMB} arcmin at 95, 150, and 220 GHz, respectively, over an effective area of ≈400 square degrees. The 220 GHz maps achieve a signal to noise on polarized dust emission approximately equal to that of Planck at 353 GHz. We take auto and cross spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz. We evaluate the joint likelihood of the spectra versus a multicomponent model of lensed-ΛCDM+r+dust+synchrotron+noise. The foreground model has seven parameters, and we impose priors on some of these using external information from Planck and WMAP derived from larger regions of sky. The model is shown to be an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r_{0.05}0.07 at 95% confidence, which tightens to r_{0.05}0.06 in conjunction with Planck temperature measurements and other data. The lensing signal is detected at 8.8σ significance. Running a maximum likelihood search on simulations we obtain unbiased results and find that σ(r)=0.020. These are the strongest constraints to date on primordial gravitational waves.

The following paper presents an approach to identify optimal roll behavior for passenger cars equipped with semiactive dampers and active electromechanical anti-roll bars. Acentral roll torque reference and a roll torque allocation interface are introduced which together allow for separated manipulation of transient and stationary roll behavior. A new subjective-objective correlation approach is presented which uses human perception models to improve matching between the objective and the subjective evaluation basis of roll dynamics to finally enable identification of optimal central roll torque reference.

Zusammenfassung Um die Bedeutung von Follikel-Lutein-(FL)-Zysten des Rindes als Sterilitatsfaktor naher zu bestimmen, wurden 22 Uteri und Ovarpaare von Schlachtrindern mit anovulatorischen luteinisierten Eierstocksblasen gesammelt, in frischem Zustand makroskopisch und spater mikroskopisch untersucht. Zehn Kuhe und 12 Farsen waren von der FL-Zystenbildung betroffen. Die meisten FL-Zysten (13) traten gleichzeitig mit einem funktionsfahigen Corpus luteum auf; sie waren durchschnittlich kleiner als die FL-Zysten ohne gleichzeitig vorkommenden funktionsfahigen Gelbkorper. Histologisch zeigten die FL-Zysten den gleichen, in verschiedene Entwicklungsstadien unterteilbaren Aufbau wie kompakte und zystose Corpora lutea. Die Mehrzahl der FL-Zysten (18 von 22) wies Ruckbildungserscheinungen auf. Bei 9 von den 13 Tieren, die zusatzlich ein funktionsfahiges Corpus luteum aufwiesen, war der Gelbkorper junger als die jeweilige FL-Zyste, und nur einmal war die FL-Zyste junger. Aus den erhobenen Befunden wurde geschlossen, das sich die FL-Zyste in der Mehrzahl der Falle zyklusgerecht zuruckbildet und das Zyklusgeschehen nicht weiter beeinflust. Es gibt aber auch Hinweise darauf, das die FL-Zyste Ausdruck eines anovulatorischen Zyklusablaufs sein kann und somit als Sterilitatsfaktor in Betracht gezogen werden mus. Summary Follice-lutein cysts in cattle. Morphology and discussion of their significance as a factor in sterility In order to look further into the significance of follice-lutein (FL) cysts as a factor in sterility 22 sets of uterus and ovaries from slaughter cattle with anovulatory luteinized ovarian cysts were collected, examined macroscopically while fresh and later examined histologically. Ten cows and 12 heifers showed FL cyst formation. Most of the FL cysts (13) were present along with a functioning corpus luteum; they were on average smaller than the FL cysts which were not accompanied by a functioning CL. Histologically, the FL cysts showed the same development stages and structure as compact and cystic CL. Most of the FL cysts (18 out of 22) showed regressive changes. In 9 of the 13 animals which showed a functioning CL the latter was younger than the corresponding FL cysts and only in one animal was the FL younger than the CL. It is concluded from these observations that the FL cysts can be an expression of an anovulatory cycle and so must be considered as a causal factor in sterility. Resume A propos du kyste folliculaire luteinique du bovin Morphologie et discussion sur sa signification en tant que facteur de sterilite 22 uterus et paires d'ovaries de bovins abattus presentant des ampoules non ovulees luteinisees ont ete recueillis puis examines macroscopiquement a l'etat frais et ensuite microscopiquement afin de cerner la signification des kystes folliculaires luteiniques (kystes-FL) du bovin en tant que facteur de sterilite. 10 vaches et 12 genisses presentaient la formation de kystes-FL. La plupart des kystes-FL (13) etaient accompagnes d'un Corpus luteum fonctionnel; ces kystes etaient en moyenne plus petits que ceux non accompagnes d'un corps jaune fonctionnel. Les kystes-FL presenterent histologiquement la meme structure divisee en differents stades de developpement que des Corpora lutea compacts et en forme de kystes. La plupart des kystes-FL (18 sur 22) presenterent des symptomes de regression. Chez 9 animaux sur 13 qui presentaient en plus un corps jaune fonctionnel, ce dernier etait plus jeune que le kyste-FL correspondant, le kyste-FL fut plus jeune dans un seul cas. Les resultats ont permis de conclure que les kystes-FL regressent en accord avec le cycle dans la majorite des cas et que la fertilite n'en est pas influencee. Il n'en demeure pas moins que les kystes-FL peuvent etre l'expression d'un cycle non ovulatoire et qu'ils doivent etre consideres dans ce cas comme l'origine d'une sterilite. Resumen Sobre el quiste folicular-luteinico de la vaca Morfologia y discusion de su importancia como factor de esterilidad Para poder determinar en detalle la significacion de los quistes foliculares-luteinicos (FL) de los vacunos, se coleccionaron 22 uteros y pares de ovarios de reses de matadero con lobulos ovaricos anovulatorios luteinizados, examinandose macroscopicamente al estado fresco y, mas adelante, con el microscopio. Diez vacas y 12 vaquillonas o anales estaban afectadas por la formacion de quistes FL. La mayoria de los quistes FL (13) aparecian simultaneos con un cuerpo luteo de capacidad funcional; por lo general, eran menores que los quistes FL sin cuerpo amarillo simultaneo que funcionase. Histologicamente mostraban los quistes FL la misma estructura, subdivisible en estadios diferentes de desarrollo, que los cuerpos amarillos compactos y quisticos. La mayoria de los quistes FL (18 de 22) presentaban sintomas de involucion. En 9 de 13 animales que presentaban un cuerpo luteo adicional, el cuerpo amarillo era mas reciente que el quiste FL respectivo, y en un caso solo el quiste FL era mas reciente. De los hallazgos ubicados se llego a la conclucion, que el quiste FL involuciona en la mayoria de los casos de forma ajustada al ciclo, sin llegar a influir mas sobre los acontecimientos relativos a la reproduccion. Aunque existen tambien indicios de que los quistes FL pueden ser expresion de un trascurso anovulatorio del ciclo, debiendose tener en cuenta como causa de esterilidad.

Zusammenfassung Die in den letzten Jahren beim Rind gehauft auftretenden Corpusluteum-Zysten werden in ihrer Mikromorphologie untersucht und mit dem Aufbau von kompakten Gelbkorpern verglichen. Die zystosen Gelbkorper konnen ebenso wie die kompakten Gelbkorper verschiedenen Zyklusstadien zugeordnet werden. Ausgehend von den morphologischen Befunden wird der Versuch unternommen, die Entstehung und die Entwicklung der zystosen Gelbkorper atiologisch zu deuten, wobei moderne endokrinologische Forschungsergebnisse in die Diskussion einbezogen werden. Summary Corpus luteum cysts in cattle Their micro-morphology and a discussion of their origin The micro-morphology of the corpus luteum cysts, which have become increasingly common in cattle in recent years, is compared with that of the compact corpus luteum. In both the cystic corpus luteum and the compact one different cyclical stages of cell development can be seen. As a result of the morphological observations an attempt is made to interpret the cause and development of the cystic corpus luteum, taking account of the results of modern endocrinological researches. Resume Les kystes du corps jaune chez la vache Micromorphologie et discussion sur leur origine On examine micromorphologiquement les kystes du corps jaune de la vache, qui se rencontrent frequemment depuis quelques annes, et on compare leur structure celle des corps jaunes compacts. Comme dans les corps jaunes compacts, on peut observer dans les corps jaunes kystiques differents stades cycliques. A partier des resultats morphologiques, on tente d'interpreter etiogiquement l'origine et le developpement des corps jaunes kystiques, en considerant dans la discussion les resultats des recherches endocrinologiques modernes. Resumen El quiste de cuerpo amarillo en la vaca Micromorfologia y discusion sobre su etiologia Los quistes de cuerpo luteo, que aparecen de forma acumulada en las vacas durante los anos ultimos, se examinan en su micromorfologia, comparandose con la estructura de los cuerpos amarillos compactos. Tanto los cuerpos amarillos quisticos como los compactos se pueden adscribir a estadios diversos del ciclo. Partiendo de los hallazgos morfologicos se intenta interpretar la etiologia y el desarrollo de los cuerpos amarillos quisticos, incorporandose en la discusion los resultados de la investigacion endocrinologica moderna.

Zusammenfassung Das Luteingewebe der Follikel-Lutein-Zyste (FL-Zyste) besitzt wesentliche histomorphologische Gemeinsamkeiten mit dem von periodischen Gelbkorpern (Clp); das histomorphologische Erscheinungsbild beider Funktionsgebilde ist mit dem Progesterongehalt im peripheren Blut korrelierbar. Auch gleichen sich ihre Luteinzellen hinsichtlich ihrer Ultrastrukturen. Daruber hinaus lase besonders das elektronenmikroskopische Bild bei FL-Zysten eine — mit dem Clp vergleichbare — grose Dynamik der An- und Ruckbildungsprozesse erkennen; dieses leitet zu dem Schlus, das die Ruckbildung bei der FL-Zyste vermutlich wie beim Clp relativ rasch eintritt. Nicht die FL-Zyste selbst, sondern die zu ihrer Entstehung fuhrenden Ursachen scheinen von Bedeutung fur das Zyklusgeschehen des Rindes zu sein. Summary The position of follicle-lutein-cysts in the development of the oestrous cycle of the cow: histological, cytological and hormone analytical studies The lutein tissue of follicle-lutein-cysts (FL-cysts) possesses the same important properties as those of the copus luteum (CL). The histomorphological picture of both functional tissues is correlated with the progesterone concentration in peripheral blood. The luteal cells of the two structures are also similar in their ultrastructure. The EM picture of FL-cysts is particularly comparable with that of the CL, both having evidence of dynamic building-up and regressive processes. This leads to the conclusion that regression of FL-cysts may well take palce as rapidly as it does in the CL. It is not the FL-cysts themselves, but the factors that are responsible for their development, which seem to be important in the cyclical events in the cow. Resume Position du kyste folliculaire luteinique dans le devenir du cycle chez le bovin: recherches histologiques, cytologiques et hormonales Le tissu luteinique du kyste folliculaire luteinique (kyste FL) possede des points communs histomorphologiques essentiels avec les corps jaunes periodiques (Clp); l'image histomorphologique des deux fonctions est en correlation avec le taux de progesterone dans le sang peripherique. Leurs cellules luteiniques se valent egalement du point de vue de leur ultrastructure. L'image au microscope electronique montre en particulier chez les kystes FL, comparable avec Clp, une forte dynamique du processus de progression et de regression; ceci permet de conclure que la regression chez le kyste FL intervient relativement avec rapidite, comme probablement chez Clp. Ce n'est pas le kyste FL lui-meme, mais les causes qui ont conduit a son developpement qui semblent etre significatives pour le devenir du cycle chez le bovin. Resumen La ubicacion del quiste folicular-luteinico en el devenir del ciclo de la vaca: estudios histologicos, citologicos y hormonoanaliticos El tejido luteinico del quiste folicular-luteinico (quiste FL) posee puntos comunes histomorfologicos esenciales con los cuerpos amarillos periodicos (Cap); la imagen histomorfologica de ambas formaciones funcionales se halla en correlacion con el contenido en progesterona en la sangre periferica. Tambien se asemejan sus celulas luteinicas desde el punto de vista de sus ultraestructuras. Ademas, la imagen al microscopio electronico permite reconocer en los quistes FL una dinamica considerable del proceso de formacion e involucion, comparable al de los Cap; esto permite sacar en conclusion que la involucion del quiste FL tal vez se realice con rapidez relativa, como en los Cap. No el quiste FL en si, sino las causas que conducen a su genesis parecen tener significacion para el devenir del ciclo en los vacunos.

Zusammenfassung Da histochemisch erfasbares Lipid im Luteingewebe sich reziprok zur Progesteronsekretion verhalt, wurde sein Nachweis herangezogen, bisher festgestellte Unterschiede in der Progesteronsekretion zwischen Tieren mit Follikel-Lutein-(FL-)Zysten und mit Corpora lutea periodica zu klaren. Wahrend der durch geringere Hormonsekretion charakterisierten An- und Ruckbildung des Luteingewebes kommt es in den grosen Luteinzellen beider Funktionsgebilde zu einer tropfenformigen Anreicherung histochemisch darstellbaren Lipids, das nicht am Stoffwechselgeschehen beteiligt ist. In der Blute des Luteingewebes, bei maximaler Progesteronsekretion, ist das Lipid durch Bindung an Protein infolge des hohen Umsatzes histochemisch grosenteils nicht erfasbar. Die kleinen Luteinzellen beherbergen wahrend der Luteingewebeentwicklung ansteigende Lipidmengen. Bei den FL-Zysten fallt neben den zyklischen Veranderungen der Lipidmenge eine die gesamte aktive Hormonsekretionsphase andauernde Anreicherung von Lipidtropfen in den lumennah gelegenen Luteinzellen auf, deren Entstehung und Bedeutung diskutiert werden. Summary Comparative lipid-histochemical studies on lutein tissue of luteinized follicle cysts and periodic corpora lutea in the cow Since histologically demonstrable lipid in lutein tissue is related reciprocally to the progesterone concentration, its detection was utilized to clarify differences in progesterone secretion found between animals with follicle-lutein (FL) cysts and those with periodic corpora lutea. During characteristic formation and regression of lutein tissue characterized by reduced hormone secretion there occurs in the large luteal cells of both functional structures an increase in droplets of histochemically demonstrable lipid that is not concerned with metabolic changes. At the time of maximal progesterone secretion of the luteal tissue, the lipid is histochemically largely not detectable because of its binding to protein as a result of its high turnover. The small luteal cells accomodate increasing amounts of lipid during luteal tissue development. In FL cysts, alongside the cyclical changes in lipid amount, a lasting enrichment of lipid droplets throughout the whole phase of hormone secretion in the lutein cells near the lumen occurs and this is discussed so far as its development and significance are concerned. Resume Recherches comparees histochimiques de lipides sur le tissu luteinique des kystes folliculaires luteiniques et Corpora lutea periodica du bovin Etant donne que le lipide detectable histochimiquement dans le tissu luteinique se comporte de facon reciproque avec la secretion de progesterone, sa mise en evidence a permis d'expliquer les differences etablies jusqu'a maintenant dans la secretion de progesterone entre des animaux avec des kystes folliculaires luteiniques (FL-) et avec Corpora lutea periodica. Pendant la formation et la regression du tissu luteinique par une secretion hormonale plus faible, il se passe un enrichissement en forme de gouttes d'un lipide, representable histochimiquement, dans les grandes cellules a luteine des deux formes de fonction qui n'est pas lie au mecanisme du metabolisme. Dans l'epanouissement du tissu luteinique lors d'une secretion maximale de progesterone, le lipide n'est pas detectable histochimiquement pour une grande part a cause d'une liaison a une proteine a la suite du debit eleve. Les petites cellules a luteine hebergent des quantites croissantes de lipide pendant le developpement du tissu luteinique. Lors de kystes-FL, ce qui frappe en dehors des modifications cycliques des quantites de lipide, c'est un enrichissement continu de la phase active totale de la secretion hormonale des gouttes de lipide dans le voisinage du lumen des cellules a luteine dont l'apparition et la signification sont discutees. Resumen Estudios lipidohistoquimicos comparados en el tejido luteinico de quistes foliculoluteinicos y cuerpos luteos periodicos en reses vacunas Puesto que el lipido en el tejido luteinico, abarcable histoquimicamente, se comporta de una manera reciproca a la secrecion de progesterona, se recurrio a su puesta en evidencia para aclarar las diferencias comprobadas hasta la fecha en la secrecion de progesterona entre los animales con quistes foliculoluteinicos (FL) y los que tienen cuerpos amarillos periodicos. Mientras que en la formacion e involucion del tejido luteinico, caracterizado por una secrecion mas escasa de hormona, se produce en las celulas luteinicas de ambas formaciones funcionales un enriquecimiento en forma de goticulas de lipido, el cual se puede identificar histoquimicamente, no interviniendo en el devenir metabolico. En la floracion del tejido luteinico, bajo secrecion maxima de progesterona, el lipido no se puede identificar histoquimicamente en su mayor parte por su union a las proteinas a causa de su metabolismo elevado. Las diminutas celulas luteinicas albergan durante el desarrollo del tejido luteinico cantidades crecientes de lipidos. En los quistes FL llaman la atencion, al lado de modificaciones ciclicas de la cantidad de lipidos, un enriquecimiento de gotas lipidas, que persistio durante toda la fase activa de secrecion hormonal, en las celulas luteinicas situadas cerca de la luz, discutiendose su genesis y significacion.

Zusammenfassung Corpora lutea periodica und FL-Zysten des Rindes unterscheiden sich in mehreren biochemischen Mesgrosen deutlich voneinander. Erhebliche Unterschiede hinsichtlich der biochemischen Parameter bestehen auch zwischen NNR und Hypophysen von Tieren mit normaler Gelbkorperentwicklung und solchen, bei denen eine FL-Zyste vorhanden ist: 1 Proteinwerte: Die Proteinkonzentration steigt wahrend der morphologischen Entwicklungsstadien der Corpora lutea kontinuierlich an; in FL-Zysten zeigt sich ein deutlich verandertes Verhalten. 2 Enzymaktivitaten: Bei hoher Aktivitat der PFK ist die SuDH in Corpora lutea periodica weniger aktiv und umgekehrt. Fur FL-Zysten gilt diese Gegenlaufigkeit nicht. In NNR, HVL und HHL von Tieren mit normaler Gelbkorperentwicklung ist die Gegenlaufigkeit von PFK und SuDH vorhanden, bei Vorliegen von FL-Zysten ist diese Gegenlaufigkeit in den genannten Organen aufgehoben. 3 Glutathion: Bei Tieren mit Corpora lutea periodica unterscheiden sich die GSH-Konzentrationen in Nebennieren und Hypophysen stark voneinander, bei Tieren mit FL-Zysten jedoch nur geringgradig. 4 Regulation der PFK: PFK zeigt in FL-Zysten hohe Aktivitat bei zahlenmasig hohem Redoxquotienten aus GSH und oxidierten Glutathionformen und verhalt sich damit so, wie dies fur andere Organe beschrieben worden ist. Summary Contribution to the biochemistry of corpora lutea periodica, FL-cysts, adrenal cortex and pituitary glands of cattle In corpora lutea periodica and in follicle lutein-cysts (FL-cysts) of cattle several biochemical parameters are clearly different. The same applies to the adrenal cortex and pituitary glands of animals with a normal development of the yellow body and of those with an FL-cyst: 1 Protein: The protein concentration in corpora lutea continuously increases during the morphological phases of development; FL-cysts behave quite differently. 2 Enzyme activities: With high activity of phosphofructokinase (PFK) in corpora lutea periodica, succinic dehydrogenase (SuDH) is less active, and vice versa. This counteractivity does not exist in FL-cysts. In the adrenal and pituitary glands of animals with normal development of the yellow body this special counter-activity of PFK- and SuDH-activity also exists; in the case of FL-cysts, it is cancelled. 3 Glutathione: In animals with corpora lutea periodica GSH-concentrations in the adrenal and pituitary glands differ markedly. In animals with FL-cysts, the difference in GSH-concentration is less. 4 Regulation of PFK: In the tissue of FL-cysts, PFK has a high activity when the redox quotient of reduced GSH and of the oxidized glutathione-moieties is also high. Thus it exhibits a behaviour such as has been described for other organs. Resume A propos de la biochimie de Corpora lutea periodica, des kystes folliculaires luteiniques, du cortex surrenal et de l'hypophyse du bovin Corpora lutea periodica et les kystes-FL du bovin se differencient les uns des autres dans differentes mesures biochimiques. Des differences marquees entre des parametres biochimiques existent egalement entre le cortex surrenal et l'hypophyse des animaux presentant un developpement normal du corps jaune et ceux montrant un kyste-FL: 1 Valeurs de proteines: La concentration des proteines augmente continuellement pendant les stades morphologiques du developpement de Corpora lutea; un comportement nettement modifie se presente dans des kystes-FL. 2 Activites enzymatiques: Su DH dans Corpora lutea periodica est moins actif et inverse lors d'une forte activite de PFK; ce contre-courant n'est pas valable pour des kystes-FL. Le contre-courant de PFK et SuDH existe dans le cortex surrenal, le lobe anterieur et posterieur de l'hypophyse avec un developpement normal du corps jaune alors qu'il est suspendu dans ces organes lors de la presence des kystes-FL. 3 Glutathion: Les concentrations de GSH dans les surrenales et l'hypophyse se differencient fortement les unes de autres chez des animaux avec Corpora lutea periodica et tres faiblement chez des animaux avec kystes-FL. 4 Regulation de PFK: PFK presente une forte activite dans des kystes-FL lors d'un quotient redox eleve a partir de GSH et de formes oxydees du glutathion et se comporte ainsi comme il a ete decrit pour d'autres organes. Resumen Contribucion a la bioquimica de los cuerpos luteos periodicos, quistes FL, glandulas anterrenales y glandulas pituitarias de vacunos Algunos parametros bioquimicos determinados en los cuerpos luteos periodicos y quistes foliculares luteinicos (FL) de vacas, son bien diferentes. Tambien existen diferencias considerables con respecto a los parametros bioquimicos entre las cortezas adrenales y las hipofisis de animales con desarrollo normal de cuerpos amarillos y aquellos que presentan un quiste FL: 1 proteinas: La concentracion de proteinas aumenta en los cuerpos amarillos continuamente durante las fases morfologicas de desarrollo; en los quistes FL se aprecia un porte muy diferente. 2 actividades enzimaticas: Con actividad elevada de la fosfofructoquinasa (FFQ) en los cuerpos amarillos periodicos, es menos activa la dehidrogenasa succinica (DHSu) y viceversa. Este contramarcha no existe en los quistes FL. En las CAR, los LAH y LPH de animales con desarrollo normal de cuerpos amarillos se encuentra presente la contramarcha de FFQ y DHSu, mientras que al diagnosticarse quistes FL queda cancelada esta contramarcha en los organos mencionados. 3 glutation: En los animales con cuerpos luteos periodicos se diferencian mucho las concentraciones de GSH en los adrenes y en las hipofisis. En los animales, en los que han sido diagnosticados quistes FL, solo es escasa la diferencia en las concentraciones GSH. 4 regulacion de la FFQ: En el tejido de quistes FL, revela de FFQ una actividad elevada cuando es crecido el cociente redox de GSH reducido y de las formas oxidadas de glutation. Esto significa un porte como el descrito en los otros organos.

Zusammenfassung Die Kopfarterien der Haussaugetiere werden in ihrem Verlauf, ihrem Versorgungsgebiet, besonders aber in ihrem Ursprung miteinander verglichen. Die Beschreibung umfast die A. carotis communis und die aus ihr in Kopfnahe sowie am Kopf entspringenden Arterien, die A. carotis externa mit ihren zum Angesicht, zur Zunge, zum Ohr und zur Schlafe ziehenden Seitenzweigen und schlieslich die A. maxillaris interna bis zu ihrer Endaufzweigung in der Fossa pterygopalatina. Dabei wurde bewust auf eine in Einzelheiten gehende Schilderung des Verlaufs der Arterien, die alle in der Nachbarschaft gelegenen Muskeln, Organe, Nerven und Venen einschliesten muste, ebenso verzichtet wie auf eine vollstandige Aufzahlung aller zum Versorgungsbereich der einzelnen Arterien und Arterienaste gehorenden Organe, Muskeln oder Knochen. Diese Angaben bringen die zitierten Spezialarbeiten in aller Ausfuhrlichkeit. Sechs farbige Abbildungen veranschaulichen den Verlauf und die Verzweigung der Arterien am Kopf der Haussaugetiere. Summary The arteries of the head in domestic animals The head arteries of domestic animals are compared in respect of their course, area of supply and especially their origin. The description embraces the common carotid artery and the arteries which stem from it near the head and in the head itself, the external carotid artery with its branches to the face, tongue, ear and temple and finally the internal maxillary artery up to its final divisions in the pterygopalatine fossa. This article is renouncing completeness of detailed descriptions of the course of the arteries, as also the enumeration of the organs, muscles and bones, which are supplied by the individual arteries and their branches. These things are given by special publications. Six coloured diagrams show the course and the distribution of the arteries of the head in domestic animals. Resume Considerations sur l'anatomie comparee des arteres de la tete des mammiferes domestiques (chat, chien, porc, boeuf, mouton, chevre, cheval) Les auteurs ont compare les arteres cephaliques des mammiferes domestiques en precisant leur trajet, les regions qu'elles irriguent et surtout leur origine. Leur description concerne l'artere carotide primitive (A. carotis communis) et les arteres qui en derivent dans la region de la tete ou dans la tete elle-meme, l'artere carotide externe (A. carotis externa) et ses ramifications conduisant a la face, a la langue, a l'oreille et aux tempes, et enfin l'artere maxillaire interne (A. maxillaris interna) jusqu'a sa division terminale dans la fosse pterygo-palatine. On renonca intentionnellement a une description detaillee du cours des arteres qui aurait du prendre en consideration tous les muscles, organes, nerfs et veines situes dans les environs, ainsi qu'a une enumeration complete des organes, muscles ou os se trouvant dans les territoires irrigues par les diverses arteres ou rameaux arteriels. Ces renseignements sont contenus en detail dans les travaux cites. Six reproductions en couleur montrent le cours et les ramifications des arteres de la tete des mammiferes domestiques. Resumen Consideraciones comparativas de las arterias cefalicas de los mamiferos domesticos (gato, perro, cerdo, vaca, oveja, cabra y caballo) Las arterias cefalicas de los mamiferos domesticos se comparan entre si en su curso, zona de aprovisionamiento y, en especial, en su origen. La descripcion comprende la a. carotida comun y las arterias que de la misma emanan en proximidades de la cabeza y en ella misma, la a. carotida externa con sus ramas laterales que irrigan la cara, lengua, oreja y sien, y, por ultimo, la a. maxilar interna hasta su ramificacion final en la fosa pterigopalatina. De forma consciente, se prescindio de la descripcion detallada del curso de las arterias, que deberia incluir los musculos, organos, nervios y venas conexas, a igual que de la enumeracion completa de los organos, musculos o huesos pertenecientes al campo de abastecimiento de las distintas arterias o ramas de las mismas. Estas indicaciones se encuentran especificadas en los trabajos especiales mencionados. Seis grabados policromos ilustran el curso y las ramificaciones de las arterias en las diversas cabezas de animales domesticos.

We present results from an analysis of all data taken by the BICEP2 & Keck Array CMB polarization experiments up to and including the 2014 observing season. This includes the first Keck Array observations at 95 GHz. The maps reach a depth of 50 nK deg in Stokes $Q$ and $U$ in the 150 GHz band and 127 nK deg in the 95 GHz band. We take auto- and cross-spectra between these maps and publicly available maps from WMAP and Planck at frequencies from 23 GHz to 353 GHz. An excess over lensed-LCDM is detected at modest significance in the 95x150 $BB$ spectrum, and is consistent with the dust contribution expected from our previous work. No significant evidence for synchrotron emission is found in spectra such as 23x95, or for correlation between the dust and synchrotron sky patterns in spectra such as 23x353. We take the likelihood of all the spectra for a multi-component model including lensed-LCDM, dust, synchrotron and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio $r$), using priors on the frequency spectral behaviors of dust and synchrotron emission from previous analyses of WMAP and Planck data in other regions of the sky. This analysis yields an upper limit $r_{0.05}, 17 pages, 18 figures, minor updates to reflect accepted version, data and figures available for download at http://bicepkeck.org/

Die Radioonkologie hat in den letzten Jahren eine rasche technische Entwicklung erlebt. Die Weiterentwicklung moderner Bestrahlungsplanungssysteme und Bestrahlungsgerate hat wesentlich zur Verbesserung der kurativen Strahlentherapie des Prostatakarzinoms beigetragen.

Die AUO (Arbeitsgemeinschaft Urologische Onkologie) und die ARO (Arbeitsgemeinschaft Radiologische Onkologie) haben in den letzten 10 Jahren drei gemeinsame Studienprojekte auf dem Gebiet des Prostatakarzinoms durchgefuhrt. Es werden die Gedanken eines Verantwortlichen zu Erfolg und Misserfolg dieser interdisziplinaren Studien vorgestellt.

Hintergrund Die moderne Hochvoltstrahlentherapie ist zweifellos mit weniger Nebenwirkungen belastet. Ob sie den fruheren konventionellen Methoden hinsichtlich der Funf-Jahres-uberlebensraten uberlegen ist, soll an genugend grosen Fallzahlen bewiesen werden.

Depleting fossil resources require changes in the current energy mix towards renewable sources. Hence, upgrading processes such as torrefaction and hydrothermal carbonization (HTC) play an important role to in-crease biomass energy density and to convert biomass into a homogeneous coal product. This study focuses on the influence of temperature, residence time and feed concentration on the energy and ash yield of the process. Experiments have been carried out in a temperature and pressure controlled batch reactor using beech wood and rice shells to determine the influence of temperature, residence time and feedstock concentration on the solid bio coal. Experiments have shown that higher temperature increases carbon content and therefore the heating value of the coal. However, due to increasing mass loss with higher temperature the energy yield of the coal is affected negatively. In-creasing residence time leads to increasing heating value and increasing energy yield. Feedstock concentration has no effect on coal properties but increases mass yield and hence the energy yield of the process. Ash yield has been found to increase with increasing concentration due to a decreased mass loss.

The study was designed to determine the distribution of oestrogen receptors (OR) and progesterone receptors (PR) in specific endometrial cell population during the oestrous cycle. Uterine biopsy samples and blood were obtained from five clinically healthy cows at Days 1 (initiation of behavioural oestrus), 8, 15 and 19 of the oestrous cycle. All animals conceived after biopsy regimen. Immunoperoxidase staining techniques at light microscopic level were used to localise OR and PR. Specific positive staining reactions for both receptors were always limited to cell nuclei. Immunoreactivity was scored semiquantitatively. In the surface epithelium, OR were detectable throughout the oestrous cycle and exhibited a significant increase from Days 8 to 15. In stromal cells and glandular epithelial cells, however, staining intensities for OR were strong at behavioural oestrus (Day 1). Significantly lower immunoreactivities were recorded at cycle Day 15. At oestrus, and to a lesser extent at Day 8, a significant gradient in oestrogen receptor content was evident, showing increasing immunoreactivity with the depth of the endometrial tissue. In surface epithelial cells, significantly more progesterone receptor immunoreactivity was evident at Day 8 as compared with Days 1, 15 and 19. In glandular epithelia, only some PR stained at oestrus, many of them occurred at Day 8 and very few could occasionally be seen at Days 15 and 19. In stromal cells, PR exhibited a somewhat different quantitative staining pattern, i.e. many occurred at Days 1, 8 and 19. A significant decrease in immunoreactivity was observed between Days 8 and 15. While occasionally recorded smooth muscle cells of the myometrium could exhibit even strong immunoreactivities for both receptors, such cells of the tunica media of blood vessels were almost devoid of OR and PR. Caruncular tissue districts, in a few cases included in biopsy specimens, did not differ substantially from intercaruncular endometrium in OR and PR contents. Endothelial cells, granulocytes and lymphocytes always were devoid of specific nuclear staining. In the present study, OR and PR contents of the bovine endometrium exhibit cell type and location specific reaction patterns during the oestrous cycle. This suggests that different cell types within this target organ can respond in a different manner to identical hormonal stimuli.

The eclipsing supersoft X-ray binary CAL 87 has been observed with Chandra on August 13/14, 2001 for nearly 100 ksec, covering two full orbital cycles and three eclipses. The shape of the eclipse light curve derived from the zeroth-order photons indicates that the size of the X-ray emission region is about 1.5 solar radii. The ACIS/LETG spectrum is completely dominated by emission lines without any noticeable continuum. The brightest emission lines are significantly redshifted and double-peaked, suggestive of emanating in a 2000 km/s wind. We model the X-ray spectrum by a mixture of recombination and resonant scattering. This allows us to deduce the temperature and luminosity of the ionizing source to be kT = 50-100 eV and L_X = 5E37 erg/s., Comment: To appear in Proceedings of IAU Coll. 194 "Compact binaries in the Galaxy and beyond" (Rev. Mex. A&A Conf. Series), eds. G. Tovmassian and E. Sion

Apocrine glands of the anal sacs in cats (Felis silvestris f. catus) were examined by transmission and scanning electron microscopy. The secretory cells exhibit a typical equipment with organelles that varied according to the season as well as the animal’s sex and state of reproduction. This can be mainly explained by seasonal differences in secretory activity. The cytological dynamics observed are, particularly, related to the smooth endoplasmic reticulum, which, for the first time, can be demonstrated in its crystalloid form in apocrine glands.

(Abridged). The cataclysmic binary V405 Peg, originally discovered as ROSAT Bright Source (RBS) 1955 (= 1RXS J230949.6+213523), shows a strong contribution from a late-type secondary star in its optical spectrum, which led Schwope et al. to suggest it to be among the nearest cataclysmic binaries. We present extensive optical observations of V405 Peg. Time-series spectroscopy shows the orbital period, Porb, to be 0.1776469(7) d (= 4.2635 hr), or 5.629 cycle/d. We classify the secondary as M3 - M4.5. Astrometry with the MDM 2.4m telescope gives a parallax 7.2 +- 1.1 milli-arcsec, and a relative proper motion of 58 mas/yr. Our best estimate of the distance yields d = 149 (+26, -20) pc. The secondary stars's radial velocity has K2 = 92 +- 3 km/s, indicating a fairly low orbital inclination if the masses are typical. Extensive I-band time-series observations in the show the system varying between a minimum brightness level of I = 14.14 and states of enhanced activity about 0.2 mag brighter. While the low-state shows an ellipsoidal modulation, an additional photometric modulation appears in the high state, with 0.1 mag amplitude and period 220-280 min. The frequency of this modulation appears to be stable for a month or so, but no single period was consistently detected from one observing season to the next. We estimate the system luminosity by combining optical measurements with the archival X-ray spectrum. The implied mass accretion rate is orders of magnitudes below the predictions for the standard angular momentum loss above the period gap. The system may possibly belong to a largely undiscovered population of hibernating CVs., Comment: 11 figures; 7 of these are .png or .jpg to save space. In press for Publications of the Astronomical Society of the Pacific

We report on the detection by Swift of GRB 080913, and subsequent optical/near-infrared follow-up observations by GROND which led to the discovery of its optical/NIR afterglow and the recognition of its high-z nature via the detection of a spectral break between the i' and z' bands. Spectroscopy obtained at the ESO-VLT revealed a continuum extending down to lambda = 9400 A, and zero flux for 7500 A < lambda, 14 pages, 7 figures, ApJ (subm)

We report results from the second and third seasons of observation with the QUaD experiment. Angular power spectra of the Cosmic Microwave Background are derived for both temperature and polarization at both 100 GHz and 150 GHz, and as cross frequency spectra. All spectra are subjected to an extensive set of jackknife tests to probe for possible systematic contamination. For the implemented data cuts and processing technique such contamination is undetectable. We analyze the difference map formed between the 100 and 150 GHz bands and find no evidence of foreground contamination in polarization. The spectra are then combined to form a single set of results which are shown to be consistent with the prevailing LCDM model. The sensitivity of the polarization results is considerably better than that of any previous experiment -- for the first time multiple acoustic peaks are detected in the E-mode power spectrum at high significance., Comment: 24 pages, 23 figures, updated to reflect published version

We constrain parity-violating interactions to the surface of last scattering using spectra from the QUaD experiment's second and third seasons of observations by searching for a possible systematic rotation of the polarization directions of CMB photons. We measure the rotation angle due to such a possible "cosmological birefringence" to be 0.55 deg. +/- 0.82 deg. (random) +/- 0.5 deg. (systematic) using QUaD's 100 and 150 GHz TB and EB spectra over the multipole range 200 < l < 2000, consistent with null, and constrain Lorentz violating interactions to < 2^-43 GeV (68% confidence limit). This is the best constraint to date on electrodynamic parity violation on cosmological scales., 4 pages, 2 figures, accepted to Physical Review Letters. Improved method, updated result and clarified language

Sphingolipids are ubiquitous and essential components of eukaryotic membranes, particularly the plasma membrane. The biosynthetic pathway for the formation of these lipid species is conserved up to the formation of sphinganine. However, a divergence is apparent in the synthesis of complex sphingolipids. In animal cells, ceramide is a substrate for sphingomyelin (SM) production via the enzyme SM synthase. In contrast, fungi utilize phytoceramide in the synthesis of inositol phosphorylceramide (IPC) catalyzed by IPC synthase. Because of the absence of a mammalian equivalent, this essential enzyme represents an attractive target for anti-fungal compounds. In common with the fungi, the kinetoplastid protozoa (and higher plants) synthesize IPC rather than SM. However, orthologues of the gene believed to encode the fungal IPC synthase (AUR1) are not readily identified in the complete genome data bases of these species. By utilizing bioinformatic and functional genetic approaches, we have isolated a functional orthologue of AUR1 in the kinetoplastids, causative agents of a range of important human diseases. Expression of this gene in a mammalian cell line led to the synthesis of an IPC-like species, strongly indicating that IPC synthase activity is reconstituted. Furthermore, the gene product can be specifically inhibited by an anti-fungal-targeting IPC synthase. We propose that the kinetoplastid AUR1 functional orthologue encodes an enzyme that defines a new class of protozoan sphingolipid synthase. The identification and characterization of the protozoan IPC synthase, an enzyme with no mammalian equivalent, will raise the possibility of developing anti-protozoal drugs with minimal toxic side affects.

We report on a search for electromagnetic and/or hadronic showers (cascades) induced by a diffuse flux of neutrinos with energies between 5 TeV and 300 TeV from extraterrestrial sources. Cascades may be produced by matter interactions of all flavors of neutrinos, and contained cascades have better energy resolution and afford better background rejection than through-going \nu_\mu-induced muons. Data taken in 1997 with the AMANDA detector were searched for events with a high-energy cascade-like signature. The observed events are consistent with expected backgrounds from atmospheric neutrinos and catastrophic energy losses from atmospheric muons. Effective volumes for all flavors of neutrinos, which allow the calculation of limits for any neutrino flux model, are presented. The limit on cascades from a diffuse flux of \nu_e+\nu_\mu+\nu_\tau+\bar{\nu}_e+\bar{\nu}_\mu+\bar{\nu}_\tau is E^2 d\Phi/dE < 9.8 x 10^{-6} GeV/(cm^2 s sr), assuming a neutrino flavor flux ratio of 1:1:1 at the detector. The limit on cascades from a diffuse flux of \nu_e+\bar{\nu}_e is E^ d\Phi/dE < 6.5 x 10{-6} GeV/(cm^2 s sr), independent of the assumed neutrino flavor flux ratio., Comment: 11 pages, 8 figures, 2 tables Submitted to Physical Review D

We report optical and near-infrared follow-up observations of GRB 011121 collected predominantly at ESO telescopes in Chile. We discover a break in the afterglow light curve after 1.3 days, which implies an initial jet opening angle of about 9 deg. The jet origin of this break is supported by the fact that the spectral energy distribution is achromatic during the first 4 days. During later phases, GRB 011121 shows significant excess emission above the flux predicted by a power law, which we interpret as additional light from an underlying supernova. In particular, the spectral energy distribution of the optical transient approximately 2 weeks after the burst is clearly not of power-law type but can be presented by a blackbody with a temperature of ~ 6000 K. The deduced parameters for the decay slope and the spectral index favor a wind scenario, i.e., an outflow into a circumburst environment shaped by the stellar wind of a massive gamma-ray burst (GRB) progenitor. Because of its low redshift of z=0.36, GRB 011121 has been the best example for the GRB-supernova connection until GRB 030329 and provides compelling evidence for a circumburster wind region expected to exist if the progenitor was a massive star.

We report optical observations of the VY Scl star BZ Cam during its previous optical low state in 1999/2000. We find drastic variations in the line profiles. Narrow-band imaging observations show that its nebula extends farther than previously known and seems to be composed of two components. We determine the [OIII] line intensity of BZ Cam's nebula to 4.8 * 10^-13 erg/cm^2/s. We discover a proper motion of BZ Cam of 25+-2 mas/yr which together with the systemic radial velocity yields a space velocity of 125 km/s. We re-interpret the nebula as being photo-ionized by hypothesized transient, luminous, supersoft X-ray emission during optical low states, and shaped by the transverse motion of BZ Cam., Comment: 8 pages with aa.sty, 8 figures, to appear in A&A