adsabs/AstroCLIMB huggingface dataset:
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: Model timescales of gas stripping and depletion. (a) Time needed for all strippable gas to be stripped, t str, as a function of d proj. To estimate the uncertainty, we use random parameters of α and n from MCMC to construct an ensemble of stripping timescales. The shading area is bordered by the 16th and 84th percentiles of the timescale distribution, indicating the 1σ uncertainty. As a reference, the t str of RPS estimated by Wang et al. (2021) is plotted. The median value is the dashed gray line, and the 16th and 84th percentiles are given as gray dotted shadings. (b) Duration of galaxies becoming gas poor, t dpl, vs. the initial Δlog M H I  at d proj = R 200. With different definitions of gas poor and different stellar mass, the relation is different. Red solid, green dashed, and purple dotted lines give the time for galaxies to reach 2σ (1.06 dex) below the mean M H I  relation, FAST detection limit, and ALFALFA detection limit, respectively. For the latter two, the results for galaxies with log (M */M ☉) of 7, 8, 9, and 10 are different. A galaxy with a higher stellar mass has a longer depletion time. The uncertainty of the red solid line is given in shading and is obtained similarly as the uncertainty in panel (a). Panel (c) is similar to panel (b), but the starting time is when d proj = 2R 200. The abscissa is the value there, too.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: Results of mocking test about the influence of H I resolution on moment (0) map analysis. Mock H I images are generated assuming a surface density profile of Wang et al. (2016) and are convolved using Gaussian kernels of different FWHM, b maj. The pixel scale is one-fifth of b maj, the same as WALLABY data. The ellipticity of the projected disk is expressed as b/a, the ratio between minor-axis and major-axis, by which points are color-coded. The abscissa is equivalent to the input ratio of projected disk’s area to the beam’s. The criterion of disk’s area being 1.52 times the beam’s is plotted as a vertical dashed cyan line. Scatters in 0.1 dex width bins are plotted in black. (a) The ratio of R H I,output measured from mock image, after correction introduced in Section 3.5, to the input R H I,input. The images are generated using random geometric parameters. (b) The ratio of f RPS measured from mock image, following Wang et al. (2021), to the f RPS directly measured using profiles. The ram pressure, disk size, and ellipticity are all true values from our H I sample, and mock b maj ranges from 3.″75 to 60″. Results of one galaxy with different beam sizes are linked with dotted gray lines, and the results using the WALLABY beam size, 30″, have red edges.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: Comparison of the luminosities (and stellar mass M *) from SDSS and DECaLS surveys. (a) The difference of magnitudes using images from two surveys plotted against SDSS magnitudes. Measurements are carried out using same apertures for consistency. DECaLS magnitudes are corrected following Dey et al. (2019). Individual measurements are plotted as translucent symbols. Triangles (circles) are high-mass (low-mass) galaxies, and blue (orange) points are g-band (r-band) measurements. Binned, σ-clipped median values and scatters are plotted for each of these four categories. A reference line of 15 mag is plotted. (b) The ratio of M *'s from two surveys plotted against SDSS results and corresponding binned, σ-clipped median values and scatters. DECaLS image of #75 is of low quality and is plotted as a cross. The separation between low- and high-mass galaxies, 109 M ☉, is plotted.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The galaxies in NE (red slashes) compared with galaxies in the same range of d proj (dark-cyan backslashes) or in the whole sample (gray dots). The distributions of the deviations from SFMS (left) and the mean M H I  relation (right) are plotted. In the left panel, two galaxies that have only lower limits of SFR are included, which makes no apparent difference to the results. In the right panel, H I nondetections are plotted as translucent patches in corresponding colors using the upper limits of M H I . The median values of Δlog SFR and H I-detected Δlog M H I  in each sample are indicated with vertical dashed lines. The results of the K-S tests between the NE sample and the whole sample and between the NE sample and the same-d proj sample are listed. For Δlog M H I , K-S tests are also performed with H I nondetections. All distributions are normalized.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The uncertainty of the fitted evolutionary path, shown as the green shaded region. The meanings of circles and semicircles are the same as those in Figure 12, and symbols with dashed edges represent galaxies with log (sSFR/yr−1) ≤ −11. Galaxies without SFR measurements are plotted as empty salmon symbols. The evolutionary path with the median values of α and n is given as a solid line. The 1σ uncertainty of the path is estimated using the bootstrap method and is plotted as as the green shaded region. The 95th percentiles and evolutionary path taking into account low-sSFR galaxies are plotted as narrow blue error bars and the dashed blue line, respectively.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The posterior probability distributions of four parameters of evolutionary path model. The probability-weighted average is plotted in orange, and the 16th, 50th, and 84th percentiles are given as black dashed lines. Above each histogram, the values of three percentiles are listed. The region on the α–n plane where the prior probability is set to 0 is bordered by blue dashed–dotted line.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The substructure map. Four substructures (C, T43798, NE, T42336) are plotted in different colors and symbols and are labeled. Several groups listed in K&T17 that share galaxies with these substructures are plotted as dashed gray circles, radii of which are corresponding R 200’s.
Paper: MAXI J0637–430: A Possible Candidate for Bulk Motion Comptonization?
Authors: Kaushik Chatterjee, Dipak Debnath, Sujoy Kumar Nath, Hsiang-Kuang Chang
Figure caption: Model-fitted unfolded NICER spectra using (a) DBB+PL, (b) TCAF, and (c) TCAF+PL models in the 0.7–10 keV energy band. For all three cases, we use tbabs to account for the interstellar absorption. All these spectra are shown from the NICER observation ID 2200950103 on MJD 58792.5.
Paper: MAXI J0637–430: A Possible Candidate for Bulk Motion Comptonization?
Authors: Kaushik Chatterjee, Dipak Debnath, Sujoy Kumar Nath, Hsiang-Kuang Chang
Figure caption: Model-fitted unfolded NICER+NuSTAR spectra using (a) DBB+PL+BMC and (b) TCAF+PL+BMC models in the 0.7–70 keV energy band. For all three cases, we use tbabs to account for the interstellar absorption. Both these spectra are shown from the combined NICER and NuSTAR observation IDs 2200950103 and 80502324002, respectively, on MJD 58792.5.
Paper: MAXI J0637–430: A Possible Candidate for Bulk Motion Comptonization?
Authors: Kaushik Chatterjee, Dipak Debnath, Sujoy Kumar Nath, Hsiang-Kuang Chang
Figure caption: Model-fitted unfolded NICER+NuSTAR spectra using (a) DBB+PL and (b) DBB+BKNPL models in the 0.7–70 keV energy band. For all three cases, we use tbabs to account for the interstellar absorption. Both these spectra are shown from the combined NICER and NuSTAR observation IDs 2200950103 and 80502324002, respectively, on MJD 58792.5.
Paper: MAXI J0637–430: A Possible Candidate for Bulk Motion Comptonization?
Authors: Kaushik Chatterjee, Dipak Debnath, Sujoy Kumar Nath, Hsiang-Kuang Chang
Figure caption: Model-fitted unfolded NICER+NuSTAR spectra using (a) TCAF+PL and (b) TCAF+BKNPL models in the 0.7–70 keV energy band. For all three cases, we use tbabs to account for the interstellar absorption. Both these spectra are shown from the combined NICER and NuSTAR observation IDs 2200950103 and 80502324002, respectively, on MJD 58792.5.
Paper: MAXI J0637–430: A Possible Candidate for Bulk Motion Comptonization?
Authors: Kaushik Chatterjee, Dipak Debnath, Sujoy Kumar Nath, Hsiang-Kuang Chang
Figure caption: Variation of daily average MAXI/GSC (a) 2–10 keV total count rate, (b) 2–4 keV and 4–10 keV count rates, and (c) HR of 4–10 keV to 2–4 keV GSC count rates throughout the entire outburst.
Paper: A Theoretical Approach to the Complex Chemical Evolution of Phosphorus in the Interstellar Medium
Authors: Marina Fernández-Ruz, Izaskun Jiménez-Serra, Jacobo Aguirre
Figure caption: Bayesian inference applied to the most important reaction rate coefficients of the model and the [PO]/[PN] ratio. (a)–(e) Prior probability distributions (thin black lines) and posterior probability distributions (PPDs, wide blue lines) obtained with Bayesian inference of the five most relevant reaction rate coefficients of our model for T = 100 K and t = 104 yr, according to observations of star-forming regions from Table 3. The center of the prior distribution is the value provided by KIDA and shown in Table 1 (dashed red lines). (f) Distribution of the [PO]/[PN] abundance ratio obtained from sampling the PPD’s of the reaction rate coefficients. The median (black line) along with its 1σ confidence interval (dashed black lines) are shown, as well as the original abundances obtained in the model with KIDA values of the rate coefficients (dotted red line), and the real abundances from clouds Orion-KL, G + 0.693-0.03 and L1157 (green, orange, and magenta lines, respectively). The P-hydrogenation fraction is f P = 0.5 in all calculations.
Paper: A Theoretical Approach to the Complex Chemical Evolution of Phosphorus in the Interstellar Medium
Authors: Marina Fernández-Ruz, Izaskun Jiménez-Serra, Jacobo Aguirre
Figure caption: Bayesian inference applied to the most important reaction rate coefficients of the model, when log-uniform prior probability distributions are used. (a)–(e) Prior probability distributions (thin black lines) and posterior probability distributions (wide blue lines) obtained with Bayesian inference of the five most relevant reaction rate coefficients of our model for T = 100 K and t = 104 yr, according to observations of star-forming regions from Table 3. The values of the reaction rate coefficients provided by KIDA and summarized in Table 1 are plotted (dashed red lines). The P-hydrogenation fraction is f P = 0.5 in all calculations.
Paper: Four Years of Type Ia Supernovae Observed by TESS: Early-time Light-curve Shapes and Constraints on Companion Interaction Models
Authors: M. M. Fausnaugh, P. J. Vallely, M. A. Tucker, C. S. Kochanek, B. J. Shappee, K. Z. Stanek, George R. Ricker, Roland Vanderspek, Manan Agarwal, Tansu Daylan, Rahul Jayaraman, Rebekah Hounsell, Daniel Muthukrishna
Figure caption: Distributions of power-law indices β 1 and β 2 (which determine the shape of the early rise and peak of the light curves, respectively), the rise time t rise = (t peak − t 0)/(1 + z), and absolute magnitude M  T . We only show the 74 SNe in the “High Dynamic Range” sample, and we only show values of t rise for the 46 SNe that TESS observed the peak (see Section 2.1 and Appendix C). The distributions of various subsets of SN are consistent with each other, and the mean values of β 1, t rise, and M  T  are consistent with the results from previous studies.
Paper: Four Years of Type Ia Supernovae Observed by TESS: Early-time Light-curve Shapes and Constraints on Companion Interaction Models
Authors: M. M. Fausnaugh, P. J. Vallely, M. A. Tucker, C. S. Kochanek, B. J. Shappee, K. Z. Stanek, George R. Ricker, Roland Vanderspek, Manan Agarwal, Tansu Daylan, Rahul Jayaraman, Rebekah Hounsell, Daniel Muthukrishna
Figure caption: Peak magnitude T peak and dynamic range ΔT of the SN sample as a function of redshift. The value of T peak is based on a parabolic fit to the peak of the light curve, and ΔT is defined as the difference between the limiting magnitude ﹩{T}_{\mathrm{lim}}﹩ and T peak (see Section 2.1). For SNe where TESS did not observe the peak, we use the maximum flux observed by TESS for T peak; these SNe are marked with open circles and represent lower limits on the peak brightness. The 10 SNe with limiting magnitudes brighter than T peak have large systematic errors early in the light curve that produce a formal 3σ limit brighter than T peak; however, a coherent SN signal is still evident at later times. These SN are marked with magenta circles. The apparent magnitude of an SN with peak absolute magnitude of −19.5 is shown by the solid black line in the left panel.
Paper: Four Years of Type Ia Supernovae Observed by TESS: Early-time Light-curve Shapes and Constraints on Companion Interaction Models
Authors: M. M. Fausnaugh, P. J. Vallely, M. A. Tucker, C. S. Kochanek, B. J. Shappee, K. Z. Stanek, George R. Ricker, Roland Vanderspek, Manan Agarwal, Tansu Daylan, Rahul Jayaraman, Rebekah Hounsell, Daniel Muthukrishna
Figure caption: Distribution of 8 hr, 3σ TESS limiting magnitudes for the sample of 307 type Ia SN light curves. The limits are derived by binning the first 2 days of the light curves to 8 hr (to avoid the SN signals), calculating the rms scatter, and converting to magnitudes with ﹩{T}_{\mathrm{lim}}=-2.5\mathrm{log}\left(3\times \mathrm{RMS}\right)+20.44﹩ (see Section 2.1). The tail of the distribution brighter than 19th mag is due to systematic errors in the light curves that increase the scatter. The tail of the distribution fainter than 21st mag is statistical noise, due to the small number of data points used to calculate the 8 hr rms scatter (typically six points or less). The average limiting magnitude is 20.01, the median is 20.02, and the mode is 20.33.
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: Summary of the effect of multiple systematic errors on the power spectra. The black curve shows the map noise estimated from an ensemble of simulations with the mapping transfer matrix corrected. For reference, the signal spectra are plotted as dashed curves for the diffuse synchrotron signal at 40 GHz (Planck Collaboration et al. 2020c; dark green) and the CMB (Planck Collaboration et al. 2020b; light green; a range of tensor-to-scalar ratio 0 < r < 0.01 is represented by the shaded green area in the BB panel), respectively. The signal spectra are convolved with the 1.5° FWHM beam window function. The solid/dotted curves are the measured positive/negative systematic bias; the curves with downward arrows represent the 2σ confidence level upper limit for systematics that are not detected given the sample variance in the simulations. Pink: systematic error from the polarization angle calibration uncertainty (Section 5.1.1). Orange: effect of a 0.1 ms bias in the detector time constants (Section 5.1.2). Red: effect of a 3 × 10−3 level beam ghosting across the focal plane (Section 5.1.3). Light blue: effect of the dipolar T-to-P leakage (Section 5.1.4). Navy blue: uncertainty in the VPM transfer function parameters. The curves indicate the maximum variation in the residual power spectra for VPM parameters drawn from the 2σ confidence interval of the VPM parameter optimization process (Section 5.1.5). The shaded regions in EE and VV highlight that these are the result of an ensemble of parameters, but are not quantitative depictions of the spread. Brown: effect of a +0.3 bias in the linear polarization spectral index assumed for demodulation (Section 5.1.5). Purple: residual E-to-B mixing due to the mapping filters after the transfer matrix correction (Section 5.1.6).
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: Ground pickup signals and the landscape around the CLASS site. The concentric annuli show the demodulated linear polarization signal (u) for a pair of detectors at the bottom edge of the focal plane (linear polarizations after demodulation have the same sign between the pair and are averaged to enhance the signal) binned in the telescope azimuth angles for the seven boresight rotations. Left: data taken prior to 2017 June when the circular baffle was not blackened. Of note is the Cerro Toco mountain peak (15° elevation) at around 45◦ in azimuth, which aligns with the peak of the u signal. For this edge detector pair, the signal from the mountain appears earlier or later in the telescope azimuth coordinates depending on the boresight rotations. Right: data from 2017 July to 2018 January, where the interior of the baffle extension was blackened, and before the replacement with the asymmetric double baffle extension and new baffle roof. The Era 2 configuration gave a reduction in ground pickup comparable to the right panel in all but the outermost detectors, regardless of the blackening state.
Paper: CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
Authors: Yunyang Li, 云炀 李, Joseph R. Eimer, Keisuke Osumi, John W. Appel, Michael K. Brewer, Aamir Ali, Charles L. Bennett, Sarah Marie Bruno, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Kevin L. Denis, Rolando Dünner, Francisco Espinoza, Thomas Essinger-Hileman, Pedro Fluxá Rojas, Kathleen Harrington, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Nathan J. Miller, Sasha Novack, Carolina Núñez, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Zhilei Xu, 智磊 徐, Lingzhen Zeng
Figure caption: Effect of dipolar T-to-P leakage. Top: the demodulated linear polarization (Stokes u) Moon maps in the VPM coordinates for a pair of detectors. In this coordinate system, the VPM wire grid is horizontal. The colors are scaled to the peak amplitude of the Moon temperature maps. The 1.54° FWHM main beam is marked by the white dashed circle. Bottom left: the differential linear polarization maps of Tau A between all +45°/−45° detectors. The maps are rotated by the Tau A polarization angle at 40 GHz (Weiland et al. 2011) so that any residual Tau-A polarization signal would appear entirely as a point source in the Stokes-Q map (denoted Q rot). Because the +45°/−45° signals are differenced, their opposite-signed dipoles (top row) average constructively. Bottom right: simulation of the dipolar leakage effect from convolving scaled WMAP Q-band temperature maps with the dipolar leakage beam from all detectors.