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501. Early-type galaxy density profiles from IllustrisTNG – I. Galaxy correlations and the impact of baryons.

Author

Wang, Yunchong, Vogelsberger, Mark, Xu, Dandan, Mao, Shude, Springel, Volker, Li, Hui, Barnes, David, Hernquist, Lars, Pillepich, Annalisa, Marinacci, Federico, Pakmor, Rüediger, Weinberger, Rainer, and Torrey, Paul

Subjects
STELLAR mass, DARK matter, ACTIVE galactic nuclei, STELLAR winds, DENSITY, REDSHIFT
Abstract

We explore the isothermal total density profiles of early-type galaxies (ETGs) in the IllustrisTNG simulation. For the selected 559 ETGs at z  = 0 with stellar masses |$10^{10.7}\, \mathrm{M}_{\odot } \leqslant M_{\ast } \leqslant 10^{11.9}\, \mathrm{M}_{\odot }$|⁠ , the total power-law slope has a mean of 〈γ′〉 = 2.011 ± 0.007 and a scatter of |$\sigma _{\gamma ^{\prime }} = 0.171$| over the radial range 0.4–4 times the stellar half-mass radius. Several correlations between γ′ and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction, and in situ -formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduces many correlation trends, and in particular, γ′ is almost constant with redshift below z  = 2. Through analysing IllustrisTNG model variations, we show that black hole kinetic winds are crucial to lowering γ′ and matching observed galaxy correlations. The effects of stellar winds on γ′ are subdominant compared to active galactic nucleus (AGN) feedback, and differ due to the presence of AGN feedback from previous works. The density profiles of the ETG dark matter haloes are well described by steeper than NFW profiles, and they are steeper in the full physics (FP) run than their counterparts in the dark matter-only (DMO) run. Their inner density slopes anticorrelate (remain constant) with the halo mass in the FP (DMO) run, and anticorrelate with the halo concentration parameter c 200 in both the types of runs. The dark matter haloes of low-mass ETGs are contracted whereas high-mass ETGs are expanded, suggesting that variations in the total density profile occur through the different halo responses to baryons. [ABSTRACT FROM AUTHOR]

Published
2020
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502. SDSS-IV MaNGA: Internal mass distributions and orbital structures of early-type galaxies and their dependence on environment.

Author

Jin, Yunpeng, Zhu, Ling, Long, R J, Mao, Shude, Wang, Lan, and van de Ven, Glenn

Subjects
GALAXIES, STELLAR mass, STELLAR orbits, DARK matter, GALACTIC dynamics
Abstract

In our earlier 2019 paper, we evaluated the reliability of Schwarzschild's orbit-superposition dynamical modelling method in estimating the internal mass distribution, intrinsic stellar shapes and orbit distributions of early-type galaxies (ETGs) taken from the Illustris cosmological simulation. We now apply the same techniques to galaxies taken from the integral-field survey Mapping Nearby Galaxies with APO (MaNGA), using a sample of 149 ETGs in the mass range of |$10^{9.90}\!-\! 10^{11.80} \, \mathrm{M}_{\odot }$| and made up of 105 central and 44 satellite galaxies. We find that low-mass ETGs with log (M */M⊙) < 11.1 have an average dark matter fraction of ∼0.2 within one effective radius R e, tend to be oblate-like, and are dominated by rotation about their minor axis. High-mass ETGs with log (M */M⊙) > 11.1 have an average dark matter fraction of ∼0.4 within one effective radius R e, tend to be prolate-like, and are dominated by rotation about their major axis and by centrophilic orbits. The changes of internal structures within one R e are dominated by the total stellar mass of the individual galaxies. We find no differences of internal structures between central and satellite ETGs for the same stellar masses. However, for similar stellar mass and colour distributions, we find that ETGs more prolate-like, or with more hot orbits, tend to have higher close neighbour counts at rp  ∼ 40 kpc. [ABSTRACT FROM AUTHOR]

Published
2020
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504. KMT-2016-BLG-1397b: KMTNET-only Discovery of a Microlens Giant Planet

Author

Zang, Weicheng, primary, Hwang, Kyu-Ha, additional, Kim, Hyoun-Woo, additional, Gould, Andrew, additional, Wang, Tianshu, additional, Zhu, Wei, additional, Mao, Shude, additional, Albrow, Michael D., additional, Chung, Sun-Ju, additional, Han, Cheongho, additional, Jung, Youn Kil, additional, Ryu, Yoon-Hyun, additional, Shin, In-Gu, additional, Shvartzvald, Yossi, additional, Yee, Jennifer C., additional, Cha, Sang-Mok, additional, Kim, Dong-Jin, additional, Kim, Seung-Lee, additional, Lee, Chung-Uk, additional, Lee, Dong-Joo, additional, Lee, Yongseok, additional, Park, Byeong-Gon, additional, and Pogge, Richard W., additional

Published
2018
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509. OGLE-2017-BLG-1130: The First Binary Gravitational Microlens Detected from Spitzer Only

Author

Wang, Tianshu, primary, Calchi Novati, S., additional, Udalski, A., additional, Gould, A., additional, Mao, Shude, additional, Zang, W., additional, Beichman, C., additional, Bryden, G., additional, Carey, S., additional, Gaudi, B. S., additional, Henderson, C. B., additional, Shvartzvald, Y., additional, Yee, J. C., additional, Mróz, P., additional, Poleski, R., additional, Skowron, J., additional, Szymański, M. K., additional, Soszyński, I., additional, Kozłowski, S., additional, Pietrukowicz, P., additional, Ulaczyk, K., additional, Pawlak, M., additional, Albrow, M. D., additional, Chung, S.-J., additional, Han, C., additional, Hwang, K.-H., additional, Jung, Y. K., additional, Ryu, Y.-H., additional, Shin, I.-G., additional, Zhu, W., additional, Cha, S.-M., additional, Kim, D.-J., additional, Kim, H.-W., additional, Kim, S.-L., additional, Lee, C.-U., additional, Lee, D.-J., additional, Lee, Y., additional, Park, B.-G., additional, and Pogge, R. W., additional

Published
2018
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511. SDSS-IV MaNGA: stellar angular momentum of about 2300 galaxies: unveiling the bimodality of massive galaxy properties

Author

Graham, Mark T, primary, Cappellari, Michele, additional, Li, Hongyu, additional, Mao, Shude, additional, Bershady, Matthew A, additional, Bizyaev, Dmitry, additional, Brinkmann, Jonathan, additional, Brownstein, Joel R, additional, Bundy, Kevin, additional, Drory, Niv, additional, Law, David R, additional, Pan, Kaike, additional, Thomas, Daniel, additional, Wake, David A, additional, Weijmans, Anne-Marie, additional, Westfall, Kyle B, additional, and Yan, Renbin, additional

Published
2018
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513. SDSS-IV MaNGA: global stellar population and gradients for about 2000 early-type and spiral galaxies on the mass–size plane

Author

Li, Hongyu, primary, Mao, Shude, additional, Cappellari, Michele, additional, Ge, Junqiang, additional, Long, R J, additional, Li, Ran, additional, Mo, H J, additional, Li, Cheng, additional, Zheng, Zheng, additional, Bundy, Kevin, additional, Thomas, Daniel, additional, Brownstein, Joel R, additional, Roman Lopes, Alexandre, additional, Law, David R, additional, and Drory, Niv, additional

Published
2018
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514. The BOSS Emission-line Lens Survey. V. Morphology and Substructure of Lensed LyαEmitters at RedshiftZ≈ 2.5 in the BELLS GALLERY

Author

Cornachione, Matthew A., primary, Bolton, Adam S., additional, Shu, Yiping, additional, Zheng, Zheng, additional, Montero-Dorta, Antonio D., additional, Brownstein, Joel R., additional, Oguri, Masamune, additional, Kochanek, Christopher S., additional, Mao, Shude, additional, Pèrez-Fournon, Ismael, additional, Marques-Chaves, Rui, additional, and Mènard, Brice, additional

Published
2018
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515. The stellar orbit distribution in present-day galaxies inferred from the CALIFA survey

Author

Zhu, Ling, primary, Ven, Glenn van de, additional, Bosch, Remco van den, additional, Rix, Hans-Walter, additional, Lyubenova, Mariya, additional, Falcón-Barroso, Jesús, additional, Martig, Marie, additional, Mao, Shude, additional, Xu, Dandan, additional, Jin, Yunpeng, additional, Obreja, Aura, additional, Grand, Robert J. J., additional, Dutton, Aaron A., additional, Macciò, Andrea V., additional, Gómez, Facundo A., additional, Walcher, Jakob C., additional, García-Benito, Rubén, additional, Zibetti, Stefano, additional, and Sánchez, Sebastian F., additional

Published
2018
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516. Clearing residual planetesimals by sweeping secular resonances in transitional disks: a lone-planet scenario for the wide gaps in debris disks around Vega and Fomalhaut

Author

Zheng, Xiaochen, Lin, Douglas N. C., Kouwenhoven, M. B. N., Mao, Shude, Zhang, Xiaojia, Zheng, Xiaochen, Lin, Douglas N. C., Kouwenhoven, M. B. N., Mao, Shude, and Zhang, Xiaojia

Abstract

Extended gaps in the debris disks of both Vega and Fomalhaut have been observed. These structures have been attributed to tidal perturbations by multiple super-Jupiter gas giant planets. Within the current observational limits, however, no such massive planets have been detected. Here we propose a less stringent `lone-planet' scenario to account for the observed structure with a single eccentric gas giant and suggest that clearing of these wide gaps is induced by its sweeping secular resonance. During the depletion of the disk gas, the planet's secular resonance propagates inward and clears a wide gap over an extended region of the disk. Although some residual intermediate-size planetesimals may remain in the gap, their surface density is too low to either produce super-Earths or lead to sufficiently frequent disruptive collisions to generate any observable dusty signatures. The main advantage of this lone-planet sweeping-secular-resonance model over the previous multiple gas giant tidal truncation scenario is the relaxed requirement on the number of gas giants. The observationally inferred upper mass limit can also be satisfied provided the hypothetical planet has a significant eccentricity. A significant fraction of solar or more massive stars bear gas giant planets with significant eccentricities. If these planets acquired their present-day kinematic properties prior to the depletion of their natal disks, their sweeping secular resonance would effectively impede the retention of neighboring planets and planetesimals over a wide range of orbital semi-major axes., Comment: 20 pages, 12 figures. Accepted for publication in ApJ

Published
2017
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517. The stellar orbit distribution in present-day galaxies inferred from the CALIFA survey

Author

Zhu, Ling, van de Ven, Glenn, Bosch, Remco van den, Rix, Hans-Walter, Lyubenova, Mariya, Falcón-Barroso, Jesús, Martig, Marie, Mao, Shude, Xu, Dandan, Jin, Yunpeng, Obreja, Aura, Grand, Robert J. J., Dutton, Aaron A., Maccio, Andrea V., Gómez, Facundo A., Walcher, Jakob C., García-Benito, Rubén, Zibetti, Stefano, Sánchez, Sebastian F., Zhu, Ling, van de Ven, Glenn, Bosch, Remco van den, Rix, Hans-Walter, Lyubenova, Mariya, Falcón-Barroso, Jesús, Martig, Marie, Mao, Shude, Xu, Dandan, Jin, Yunpeng, Obreja, Aura, Grand, Robert J. J., Dutton, Aaron A., Maccio, Andrea V., Gómez, Facundo A., Walcher, Jakob C., García-Benito, Rubén, Zibetti, Stefano, and Sánchez, Sebastian F.

Abstract

Galaxy formation entails the hierarchical assembly of mass, along with the condensation of baryons and the ensuing, self-regulating star formation. The stars form a collisionless system whose orbit distribution retains dynamical memory that can constrain a galaxy's formation history. The ordered-rotation dominated orbits with near maximum circularity $\lambda_z \simeq1$ and the random-motion dominated orbits with low circularity $\lambda_z \simeq0$ are called kinematically cold and kinematically hot, respectively. The fraction of stars on `cold' orbits, compared to the fraction of stars on `hot' orbits, speaks directly to the quiescence or violence of the galaxies' formation histories. Here we present such orbit distributions, derived from stellar kinematic maps via orbit-based modelling for a well defined, large sample of 300 nearby galaxies. The sample, drawn from the CALIFA survey, includes the main morphological galaxy types and spans the total stellar mass range from $10^{8.7}$ to $10^{11.9}$ solar masses. Our analysis derives the orbit-circularity distribution as a function of galaxy mass, $p(\lambda_z~|~M_\star)$, and its volume-averaged total distribution, $p(\lambda_z)$. We find that across most of the considered mass range and across morphological types, there are more stars on `warm' orbits defined as $0.25\le \lambda_z \le 0.8$ than on either `cold' or `hot' orbits. This orbit-based "Hubble diagram" provides a benchmark for galaxy formation simulations in a cosmological context., Comment: Published in Nature Astronomy, 1 January 2018; doi:10.1038/s41550-017-0348-1; 22pages, 8 figures, 2 tables

Published
2017

518. Chemical abundances and ages of the bulge stars in APOGEE high-velocity peaks

Author

Zhou, Yingying, Shen, Juntai, Liu, Chao, Li, Zhao-Yu, Mao, Shude, Kunder, Andrea, Rich, R. Michael, Zasowski, G., Fernandez-Trincado, J. G., Majewski, Steven R., Lin, Chien-Cheng, Geisler, Doug, Tang, Baitian, Villanova, S., Roman-Lopes, A., Schultheis, M., Nidever, David L., Meza, Andrés, Pan, Kaike, Bizyaev, D. V., Zhou, Yingying, Shen, Juntai, Liu, Chao, Li, Zhao-Yu, Mao, Shude, Kunder, Andrea, Rich, R. Michael, Zasowski, G., Fernandez-Trincado, J. G., Majewski, Steven R., Lin, Chien-Cheng, Geisler, Doug, Tang, Baitian, Villanova, S., Roman-Lopes, A., Schultheis, M., Nidever, David L., Meza, Andrés, Pan, Kaike, and Bizyaev, D. V.

Abstract

A cold high-velocity (HV, $\sim$ 200 km/s) peak was first reported in several Galactic bulge fields based on the APOGEE commissioning observations. Both the existence and the nature of the high-velocity peak are still under debate. Here we revisit this feature with the latest APOGEE DR13 data. We find that most of the low latitude bulge fields display a skewed Gaussian distribution with a HV shoulder. However, only 3 out of 53 fields show distinct high-velocity peaks around 200 km/s. The velocity distribution can be well described by Gauss-Hermite polynomials, except the three fields showing clear HV peaks. We find that the correlation between the skewness parameter ($h_{3}$) and the mean velocity ($\bar{v}$), instead of a distinctive HV peak, is a strong indicator of the bar. It was recently suggested that the HV peak is composed of preferentially young stars. We choose three fields showing clear HV peaks to test this hypothesis using the metallicity, [$\alpha$/M] and [C/N] as age proxies. We find that both young and old stars show HV features. The similarity between the chemical abundances of stars in the HV peaks and the main component indicates that they are not systematically different in terms of chemical abundance or age. In contrast, there are clear differences in chemical space between stars in the Sagittarius dwarf and the bulge stars. The strong HV peaks off-plane are still to be explained properly, and could be different in nature., Comment: 13 pages, 10 figures, published in ApJ. Updated to match the final ApJ published version. Minor revisions to the text and Figure 4

Published
2017
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519. The Origins of UV-optical Color Gradients in Star-forming Galaxies at z ~ 2: Predominant Dust Gradients But Negligible sSFR Gradients

Author

Liu, F. S., Jiang, Dongfei, Faber, S. M., Koo, David C., Yesuf, Hassen M., Tacchella, Sandro, Mao, Shude, Wang, Weichen, Guo, Yicheng, Fang, Jerome J., Barro, Guillermo, Zheng, Xianzhong, Jia, Meng, Tong, Wei, Liu, Lu, Meng, Xianmin, Liu, F. S., Jiang, Dongfei, Faber, S. M., Koo, David C., Yesuf, Hassen M., Tacchella, Sandro, Mao, Shude, Wang, Weichen, Guo, Yicheng, Fang, Jerome J., Barro, Guillermo, Zheng, Xianzhong, Jia, Meng, Tong, Wei, Liu, Lu, and Meng, Xianmin

Abstract

The rest-frame UV-optical (i.e., $NUV-B$) color is sensitive to both low-level recent star formation (specific star formation rate - sSFR) and dust. In this Letter, we extend our previous work on the origins of $NUV-B$ color gradients in star-forming galaxies (SFGs) at $z\sim1$ to those at $z\sim2$. We use a sample of 1335 large (semi-major axis radius $R_{\rm SMA}>0.''18$) SFGs with extended UV emission out to $2R_{\rm SMA}$ in the mass range $M_{\ast} = 10^{9}-10^{11}M_{\odot}$ at $1.5

Published
2017
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520. The origin and properties of massive prolate galaxies in the Illustris simulation

Author

Li, Hongyu, Mao, Shude, Emsellem, Eric, Xu, Dandan, Springel, Volker, Krajnović, Davor, Li, Hongyu, Mao, Shude, Emsellem, Eric, Xu, Dandan, Springel, Volker, and Krajnović, Davor

Abstract

We study galaxy shapes in the Illustris cosmological hydrodynamic simulation. We find that massive galaxies have a higher probability of being prolate. For galaxies with stellar mass larger than $10^{11}\rm M_{\odot}$, 35 out of total 839 galaxies are prolate. For 21 galaxies with stellar mass larger than $10^{12}\rm M_{\odot}$, 9 are prolate, 4 are triaxial while the others are close to being oblate. There are almost no prolate galaxies with stellar mass smaller than $3\times10^{11}\rm M_{\odot}$. We check the merger history of the prolate galaxies, and find that they are formed by major dry mergers. All the prolate galaxies have at least one such merger, with most having mass ratios between $1:1$ and $1:3$. The gas fraction (gas mass to total baryon mass) of the progenitors is 0-3 percent for nearly all these mergers, except for one whose second progenitor contains $\sim 15\%$ gas mass, while its main progenitor still contains less than $5\%$. For the 35 massive prolate galaxies that we find, 18 of them have minor axis rotation, and their angular momenta mostly come from the spin angular momenta of the progenitors (usually that of the main progenitor). We analyse the merger orbits of these prolate galaxies and find that most of them experienced a nearly radial merger orbit. Oblate galaxies with major dry mergers can have either radial or circular merger orbits. We further discuss various properties of these prolate galaxies, such as spin parameter $\lambda_{\rm R}$, spherical anisotropy parameter $\beta$, dark matter fraction, as well as inner density slopes for the stellar, dark matter and total mass distributions., Comment: Accepted for publication in MNRAS. 24 pages, 14 figures

Published
2017
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521. PHL 6625: A Minor Merger-Associated QSO Behind NGC 247

Author

Tao, Lian, Feng, Hua, Shen, Yue, Ho, Luis C., Ge, Junqiang, Kaaret, Philip, Mao, Shude, Liu, Xin, Tao, Lian, Feng, Hua, Shen, Yue, Ho, Luis C., Ge, Junqiang, Kaaret, Philip, Mao, Shude, and Liu, Xin

Abstract

PHL 6625 is a luminous quasi-stellar object (QSO) at z = 0.3954 located behind the nearby galaxy NGC 247 (z = 0.0005). Hubble Space Telescope (HST) observations revealed an arc structure associated with it. We report on spectroscopic observations with the Very Large Telescope (VLT) and multiwavelength observations from the radio to the X-ray band for the system, suggesting that PHL 6625 and the arc are a close pair of merging galaxies, instead of a strong gravitational lens system. The QSO host galaxy is estimated to be (4-28) x 10^10 M_sun, and the mass of the companion galaxy of is estimated to be M_* = (6.8 +/- 2.4) x 10^9 M_sun, suggesting that this is a minor merger system. The QSO displays typical broad emission lines, from which a black hole mass of about (2-5) x 10^8 M_sun and an Eddington ratio of about 0.01-0.05 can be inferred. The system represents an interesting and rare case where a QSO is associated with an ongoing minor merger, analogous to Arp 142., Comment: ApJ to appear

Published
2017
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522. SDSS-IV MaNGA: variation of the stellar initial mass function in spiral and early-type galaxies

Author

Li, Hongyu, Ge, Junqiang, Mao, Shude, Cappellari, Michele, Long, R. J., Li, Ran, Emsellem, Eric, Dutton, Aaron A., Li, Cheng, Bundy, Kevin, Thomas, Daniel, Drory, Niv, Lopes, Alexandre Roman, Li, Hongyu, Ge, Junqiang, Mao, Shude, Cappellari, Michele, Long, R. J., Li, Ran, Emsellem, Eric, Dutton, Aaron A., Li, Cheng, Bundy, Kevin, Thomas, Daniel, Drory, Niv, and Lopes, Alexandre Roman

Abstract

We perform Jeans anisotropic modeling (JAM) on elliptical and spiral galaxies from the MaNGA DR13 sample. By comparing the stellar mass-to-light ratios estimated from stellar population synthesis (SPS) and from JAM, we find a similar systematic variation of the initial mass function (IMF) as in the earlier $\rm ATLAS^{3D}$ results. Early type galaxies (elliptical and lenticular) with lower velocity dispersions within one effective radius are consistent with a Chabrier-like IMF while galaxies with higher velocity dispersions are consistent with a more bottom heavy IMF such as the Salpeter IMF. Spiral galaxies have similar systematic IMF variations, but with slightly different slopes and larger scatters, due to the uncertainties caused by higher gas fractions and extinctions for these galaxies. Furthermore, we examine the effects of stellar mass-to-light ratio gradients on our JAM modeling, and find that the trends from our results becomes stronger after considering the gradients., Comment: Accepted for publication in ApJ. 9 pages, 9 figures

Published
2017
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523. UVI colour gradients of 0.4<z<1.4 star-forming main sequence galaxies in CANDELS: dust extinction and star formation profiles

Author

Wang, Weichen, Faber, S. M., Liu, F. S., Guo, Yicheng, Pacifici, Camilla, Koo, David C., Kassin, Susan A., Mao, Shude, Fang, Jerome J., Chen, Zhu, Koekemoer, Anton M., Kocevski, Dale D., Ashby, M. L. N., Wang, Weichen, Faber, S. M., Liu, F. S., Guo, Yicheng, Pacifici, Camilla, Koo, David C., Kassin, Susan A., Mao, Shude, Fang, Jerome J., Chen, Zhu, Koekemoer, Anton M., Kocevski, Dale D., and Ashby, M. L. N.

Abstract

This paper uses radial colour profiles to infer the distributions of dust, gas and star formation in z=0.4-1.4 star-forming main sequence galaxies. We start with the standard UVJ-based method to estimate dust extinction and specific star formation rate (sSFR). By replacing J with I band, a new calibration method suitable for use with ACS+WFC3 data is created (i.e. UVI diagram). Using a multi-wavelength multi-aperture photometry catalogue based on CANDELS, UVI colour profiles of 1328 galaxies are stacked in stellar mass and redshift bins. The resulting colour gradients, covering a radial range of 0.2--2.0 effective radii, increase strongly with galaxy mass and with global $A_V$. Colour gradient directions are nearly parallel to the Calzetti extinction vector, indicating that dust plays a more important role than stellar population variations. With our calibration, the resulting $A_V$ profiles fall much more slowly than stellar mass profiles over the measured radial range. sSFR gradients are nearly flat without central quenching signatures, except for $M_*>10^{10.5} M_{\odot}$, where central declines of 20--25 per cent are observed. Both sets of profiles agree well with previous radial sSFR and (continuum) $A_V$ measurements. They are also consistent with the sSFR profiles and, if assuming a radially constant gas-to-dust ratio, gas profiles in recent hydrodynamic models. We finally discuss the striking findings that SFR scales with stellar mass density in the inner parts of galaxies, and that dust content is high in the outer parts despite low stellar-mass surface densities there., Comment: 22 pages, 16 figures, accepted by MNRAS for publication

Published
2017
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524. Torus Models of the Outer Disc of the Milky Way using LAMOST Survey Data

Author

Wang, Qiao, Wang, Yougang, Liu, Chao, Mao, Shude, Long, R. J., Wang, Qiao, Wang, Yougang, Liu, Chao, Mao, Shude, and Long, R. J.

Abstract

With a sample of 48,161 K giant stars selected from the LAMOST DR 2 catalogue, we construct torus models in a large volume extending, for the first time, from the solar vicinity to a Galactocentric distance of $\sim 20$ kpc, reaching the outskirts of the Galactic disc. We show that the kinematics of the K giant stars match conventional models, e.g. as created by Binney in 2012, in the Solar vicinity. However such two-disc models fail if they are extended to the outer regions, even if an additional disc component is utilised. If we loosen constraints in the Sun's vicinity, we find that an effective thick disc model could explain the anti-centre of the MW. The LAMOST data imply that the sizes of the Galactic discs are much larger, and that the outer disc is much thicker, than previously thought, or alternatively that the outer structure is not a conventional disc at all. However, the velocity dispersion $\sigma_{0z}$ of the kinematically thick disc in the best-fitting model is about 80 km s$^{-1}$ and has a scale parameter $R_{\sigma}$ for an exponential distribution function of $\sim 19$ kpc. Such a height $\sigma_{0z}$ is strongly rejected by current measurements in the solar neighbourhood, and thus a model beyond quasi-thermal, two or three thin or thick discs is required., Comment: 11 pages, 7 figures and 3 tables, Accepted for publication in MNRAS

Published
2017
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525. MOA-2016-BLG-227Lb: A Massive Planet Characterized by Combining Lightcurve Analysis and Keck AO Imaging

Author

Koshimoto, Naoki, Shvartzvald, Yossi, Bennett, David, Penny, Matthew, Hundertmark, Markus, Bond, Ian A., Zang, Weicheng, Henderson, Calen, Suzuki, Daisuke, Rattenbury, Nicholas J., Sumi, Takahiro, Abe, Fumio, Asakura, Yuichiro, Bhattacharya, Aparna, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Li, M. C. A., Ling, C., Masuda, Kimiaki, Matsubara, Y., Matsuo, Taro, Muraki, Yasushi, Nagakane, Masayuki, Ohnishi, Kouji, Ranc, C., Saito, To., Sharan, A., Shibai, Hiroshi, Sullivan, Denis, Tristram, P., Yonehara, A., Gelino, Christopher, Beichman, Charles, Beaulieu, Jean-Philippe, Marquette, J. -B., Batista, Virginie, Friedmann, M., Hallakoun, N., Kaspi, Shai, Maoz, Dani, Bryden, G., Novati, Sebastiano Calchi, Howell, Steve, Wang, T., Mao, Shude, Fouque, Pascal, Korhonen, Heidi, Jorgensen, Uffe, Street, Rachel, Tsapras, Yiannis, Dominik, Martin, Kerins, Eamonn, Cassan, Arnaud, Snodgrass, Colin, Bachelet, Etienne, Bozza, Valerio, Bramich, D. M., Koshimoto, Naoki, Shvartzvald, Yossi, Bennett, David, Penny, Matthew, Hundertmark, Markus, Bond, Ian A., Zang, Weicheng, Henderson, Calen, Suzuki, Daisuke, Rattenbury, Nicholas J., Sumi, Takahiro, Abe, Fumio, Asakura, Yuichiro, Bhattacharya, Aparna, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Li, M. C. A., Ling, C., Masuda, Kimiaki, Matsubara, Y., Matsuo, Taro, Muraki, Yasushi, Nagakane, Masayuki, Ohnishi, Kouji, Ranc, C., Saito, To., Sharan, A., Shibai, Hiroshi, Sullivan, Denis, Tristram, P., Yonehara, A., Gelino, Christopher, Beichman, Charles, Beaulieu, Jean-Philippe, Marquette, J. -B., Batista, Virginie, Friedmann, M., Hallakoun, N., Kaspi, Shai, Maoz, Dani, Bryden, G., Novati, Sebastiano Calchi, Howell, Steve, Wang, T., Mao, Shude, Fouque, Pascal, Korhonen, Heidi, Jorgensen, Uffe, Street, Rachel, Tsapras, Yiannis, Dominik, Martin, Kerins, Eamonn, Cassan, Arnaud, Snodgrass, Colin, Bachelet, Etienne, Bozza, Valerio, and Bramich, D. M.

Abstract

We report the discovery of a microlensing planet --- MOA-2016-BLG-227Lb --- with a large planet/host mass ratio of $q \simeq 9 \times 10^{-3}$. This event was located near the $K2$ Campaign 9 field that was observed by a large number of telescopes. As a result, the event was in the microlensing survey area of a number of these telescopes, and this enabled good coverage of the planetary light curve signal. High angular resolution adaptive optics images from the Keck telescope reveal excess flux at the position of the source above the flux of the source star, as indicated by the light curve model. This excess flux could be due to the lens star, but it could also be due to a companion to the source or lens star, or even an unrelated star. We consider all these possibilities in a Bayesian analysis in the context of a standard Galactic model. Our analysis indicates that it is unlikely that a large fraction of the excess flux comes from the lens, unless solar type stars are much more likely to host planets of this mass ratio than lower mass stars. We recommend that a method similar to the one developed in this paper be used for other events with high angular resolution follow-up observations when the follow-up observations are insufficient to measure the lens-source relative proper motion., Comment: 35 pages, 7 figures, 6 tables, Accepted for publication in AJ

Published
2017
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526. Project Overview of the Beijing-Arizona Sky Survey

Author

Zou, Hu, Zhou, Xu, Fan, Xiaohui, Zhang, Tianmeng, Zhou, Zhimin, Nie, Jundan, Peng, Xiyan, McGreer, Ian, Jiang, Linhua, Dey, Arjun, Fan, Dongwei, He, Boliang, Jiang, Zhaoji, Lang, Dustin, Lesser, Michael, Ma, Jun, Mao, Shude, Schlegel, David, Wang, Jiali, Zou, Hu, Zhou, Xu, Fan, Xiaohui, Zhang, Tianmeng, Zhou, Zhimin, Nie, Jundan, Peng, Xiyan, McGreer, Ian, Jiang, Linhua, Dey, Arjun, Fan, Dongwei, He, Boliang, Jiang, Zhaoji, Lang, Dustin, Lesser, Michael, Ma, Jun, Mao, Shude, Schlegel, David, and Wang, Jiali

Abstract

The Beijing-Arizona Sky Survey (BASS) is a wide-field two-band photometric survey of the Northern Galactic Cap using the 90Prime imager on the 2.3 m Bok telescope at Kitt Peak. It is a four-year collaboration between the National Astronomical Observatory of China and Steward Observatory, the University of Arizona, serving as one of the three imaging surveys to provide photometric input catalogs for target selection of the Dark Energy Spectroscopic Instrument (DESI) project. BASS will take up to 240 dark/grey nights to cover an area of about 5400 deg$^2$ in the $g$ and $r$ bands. The 5$\sigma$ limiting AB magnitudes for point sources in the two bands, corrected for the Galactic extinction, are 24.0 and 23.4 mag, respectively. BASS, together with other DESI imaging surveys, will provide unique science opportunities that cover a wide range of topics in both Galactic and extragalactic astronomy., Comment: 10 pages, submitted to PASP

Published
2017
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527. The First Data Release of the Beijing-Arizona Sky Survey

Author

Zou, Hu, Zhang, Tianmeng, Zhou, Zhimin, Nie, Jundan, Peng, Xiyan, Zhou, Xu, Jiang, Linhua, Cai, Zheng, Dey, Arjun, Fan, Xiaohui, Fan, Dongwei, Guo, Yucheng, He, Boliang, Jiang, Zhaoji, Lang, Dustin, Lesser, Michael, Li, Zefeng, Ma, Jun, Mao, Shude, McGreer, Ian, Schlegel, David, Shao, Yali, Wang, Jiali, Wang, Shu, Wu, Jin, Wu, Xiaohan, Yang, Qian, Yue, Minghao, Zou, Hu, Zhang, Tianmeng, Zhou, Zhimin, Nie, Jundan, Peng, Xiyan, Zhou, Xu, Jiang, Linhua, Cai, Zheng, Dey, Arjun, Fan, Xiaohui, Fan, Dongwei, Guo, Yucheng, He, Boliang, Jiang, Zhaoji, Lang, Dustin, Lesser, Michael, Li, Zefeng, Ma, Jun, Mao, Shude, McGreer, Ian, Schlegel, David, Shao, Yali, Wang, Jiali, Wang, Shu, Wu, Jin, Wu, Xiaohan, Yang, Qian, and Yue, Minghao

Abstract

The Beijing-Arizona Sky Survey (BASS) is a new wide-field legacy imaging survey in the northern Galactic cap using the 2.3m Bok telescope. The survey will cover about 5400 deg$^2$ in the $g$ and $r$ bands, and the expected 5$\sigma$ depths (corrected for the Galactic extinction) in the two bands are 24.0 and 23.4 mag, respectively. BASS started observations in January 2015, and has completed about 41% of the whole area as of July 2016. The first data release contains both calibrated images and photometric catalogs obtained in 2015 and 2016. The depths of single-epoch images in the two bands are 23.4 and 22.9 mag, and the full depths of three epochs are about 24.1 and 23.5 mag, respectively., Comment: 16 pages, published by AJ

Published
2017
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528. Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe

Author

Blanton, Michael R., Bershady, Matthew A., Abolfathi, Bela, Albareti, Franco D., Prieto, Carlos Allende, Almeida, Andres, Alonso-García, Javier, Anders, Friedrich, Anderson, Scott F., Andrews, Brett, Aquino-Ortíz, Erik, Aragón-Salamanca, Alfonso, Argudo-Fernández, Maria, Armengaud, Eric, Aubourg, Eric, Avila-Reese, Vladimir, Badenes, Carles, Bailey, Stephen, Barger, Kathleen A., Barrera-Ballesteros, Jorge, Bartosz, Curtis, Bates, Dominic, Baumgarten, Falk, Bautista, Julian, Beaton, Rachael, Beers, Timothy C., Belfiore, Francesco, Bender, Chad F., Berlind, Andreas A., Bernardi, Mariangela, Beutler, Florian, Bird, Jonathan C., Bizyaev, Dmitry, Blanc, Guillermo A., Blomqvist, Michael, Bolton, Adam S., Boquien, Médéric, Borissova, Jura, Bosch, Remco van den, Bovy, Jo, Brandt, William N., Brinkmann, Jonathan, Brownstein, Joel R., Bundy, Kevin, Burgasser, Adam J., Burtin, Etienne, Busca, Nicolás G., Cappellari, Michele, Carigi, Maria Leticia Delgado, Carlberg, Joleen K., Rosell, Aurelio Carnero, Carrera, Ricardo, Cherinka, Brian, Cheung, Edmond, Chew, Yilen Gómez Maqueo, Chiappini, Cristina, Choi, Peter Doohyun, Chojnowski, Drew, Chuang, Chia-Hsun, Chung, Haeun, Cirolini, Rafael Fernando, Clerc, Nicolas, Cohen, Roger E., Comparat, Johan, da Costa, Luiz, Cousinou, Marie-Claude, Covey, Kevin, Crane, Jeffrey D., Croft, Rupert A. C., Cruz-Gonzalez, Irene, Cuadra, Daniel Garrido, Cunha, Katia, Damke, Guillermo J., Darling, Jeremy, Davies, Roger, Dawson, Kyle, de la Macorra, Axel, De Lee, Nathan, Delubac, Timothée, Di Mille, Francesco, Diamond-Stanic, Aleks, Cano-Díaz, Mariana, Donor, John, Downes, Juan José, Drory, Niv, Bourboux, Hélion du Mas des, Duckworth, Christopher J., Dwelly, Tom, Dyer, Jamie, Ebelke, Garrett, Eisenstein, Daniel J., Emsellem, Eric, Eracleous, Mike, Escoffier, Stephanie, Evans, Michael L., Fan, Xiaohui, Fernández-Alvar, Emma, Fernandez-Trincado, J. G., Feuillet, Diane K., Finoguenov, Alexis, Fleming, Scott W., Font-Ribera, Andreu, Fredrickson, Alexander, Freischlad, Gordon, Frinchaboy, Peter M., Galbany, Lluís, Garcia-Dias, R., García-Hernández, D. A., Gaulme, Patrick, Geisler, Doug, Gelfand, Joseph D., Gil-Marín, Héctor, Gillespie, Bruce A., Goddard, Daniel, Gonzalez-Perez, Violeta, Grabowski, Kathleen, Green, Paul J., Grier, Catherine J., Gunn, James E., Guo, Hong, Guy, Julien, Hagen, Alex, Hahn, ChangHoon, Hall, Matthew, Harding, Paul, Hasselquist, Sten, Hawley, Suzanne L., Hearty, Fred, Hernández, Jonay I. Gonzalez, Ho, Shirley, Hogg, David W., Holley-Bockelmann, Kelly, Holtzman, Jon A., Holzer, Parker H., Huehnerhoff, Joseph, Hutchinson, Timothy A., Hwang, Ho Seong, Ibarra-Medel, Héctor J., Ilha, Gabriele da Silva, Ivans, Inese I., Ivory, KeShawn, Jackson, Kelly, Jensen, Trey W., Johnson, Jennifer A., Jones, Amy, Jönsson, Henrik, Jullo, Eric, Kamble, Vikrant, Kinemuchi, Karen, Kirkby, David, Kitaura, Francisco-Shu, Klaene, Mark, Knapp, Gillian R., Kneib, Jean-Paul, Kollmeier, Juna A., Lacerna, Ivan, Lane, Richard R., Lang, Dustin, Law, David R., Lazarz, Daniel, Goff, Jean-Marc Le, Liang, Fu-Heng, Li, Cheng, LI, Hongyu, Lima, Marcos, Lin, Lihwai, Lin, Yen-Ting, de Lis, Sara Bertran, Liu, Chao, Lizaola, Miguel Angel C. de Icaza, Long, Dan, Lucatello, Sara, Lundgren, Britt, MacDonald, Nicholas K., Machado, Alice Deconto, MacLeod, Chelsea L., Mahadevan, Suvrath, Maia, Marcio Antonio Geimba, Maiolino, Roberto, Majewski, Steven R., Malanushenko, Elena, Malanushenko, Viktor, Manchado, Arturo, Mao, Shude, Maraston, Claudia, Marques-Chaves, Rui, Masters, Karen L., McBride, Cameron K., McDermid, Richard M., McGrath, Brianne, McGreer, Ian D., Peña, Nicolás Medina, Melendez, Matthew, Merloni, Andrea, Merrifield, Michael R., Meszaros, Szabolcs, Meza, Andres, Minchev, Ivan, Minniti, Dante, Miyaji, Takamitsu, More, Surhud, Mulchaey, John, Müller-Sánchez, Francisco, Muna, Demitri, Munoz, Ricardo R., Myers, Adam D., Nair, Preethi, Nandra, Kirpal, Nascimento, Janaina Correa do, Negrete, Alenka, Ness, Melissa, Newman, Jeffrey A., Nichol, Robert C., Nidever, David L., Nitschelm, Christian, Ntelis, Pierros, O'Connell, Julia E., Oelkers, Ryan J., Oravetz, Audrey, Oravetz, Daniel, Pace, Zach, Padilla, Nelson, Palanque-Delabrouille, Nathalie, Palicio, Pedro Alonso, Pan, Kaike, Parikh, Taniya, Pâris, Isabelle, Park, Changbom, Patten, Alim Y., Peirani, Sebastien, Pellejero-Ibanez, Marcos, Penny, Samantha, Percival, Will J., Perez-Fournon, Ismael, Petitjean, Patrick, Pieri, Matthew M., Pinsonneault, Marc, Pisani, Alice, Poleski, Radosław, Prada, Francisco, Prakash, Abhishek, Queiroz, Anna Bárbara de Andrade, Raddick, M. Jordan, Raichoor, Anand, Rembold, Sandro Barboza, Richstein, Hannah, Riffel, Rogemar A., Riffel, Rogério, Rix, Hans-Walter, Robin, Annie C., Rockosi, Constance M., Rodríguez-Torres, Sergio, Roman-Lopes, A., Román-Zúñiga, Carlos, Rosado, Margarita, Ross, Ashley J., Rossi, Graziano, Ruan, John, Ruggeri, Rossana, Rykoff, Eli S., Salazar-Albornoz, Salvador, Salvato, Mara, Sánchez, Ariel G., Aguado, David Sánchez, Sánchez-Gallego, José R., Santana, Felipe A., Santiago, Basílio Xavier, Sayres, Conor, Schiavon, Ricardo P., Schimoia, Jaderson da Silva, Schlafly, Edward F., Schlegel, David J., Schneider, Donald P., Schultheis, Mathias, Schuster, William J., Schwope, Axel, Seo, Hee-Jong, Shao, Zhengyi, Shen, Shiyin, Shetrone, Matthew, Shull, Michael, Simon, Joshua D., Skinner, Danielle, Skrutskie, M. F., Slosar, Anže, Smith, Verne V., Sobeck, Jennifer S., Sobreira, Flavia, Somers, Garrett, Souto, Diogo, Stark, David V., Stassun, Keivan, Stauffer, Fritz, Steinmetz, Matthias, Storchi-Bergmann, Thaisa, Streblyanska, Alina, Stringfellow, Guy S., Suárez, Genaro, Sun, Jing, Suzuki, Nao, Szigeti, Laszlo, Taghizadeh-Popp, Manuchehr, Tang, Baitian, Tao, Charling, Tayar, Jamie, Tembe, Mita, Teske, Johanna, Thakar, Aniruddha R., Thomas, Daniel, Thompson, Benjamin A., Tinker, Jeremy L., Tissera, Patricia, Tojeiro, Rita, Toledo, Hector Hernandez, de la Torre, Sylvain, Tremonti, Christy, Troup, Nicholas W., Valenzuela, Octavio, Valpuesta, Inma Martinez, Vargas-González, Jaime, Vargas-Magaña, Mariana, Vazquez, Jose Alberto, Villanova, Sandro, Vivek, M., Vogt, Nicole, Wake, David, Walterbos, Rene, Wang, Yuting, Weaver, Benjamin Alan, Weijmans, Anne-Marie, Weinberg, David H., Westfall, Kyle B., Whelan, David G., Wild, Vivienne, Wilson, John, Wood-Vasey, W. M., Wylezalek, Dominika, Xiao, Ting, Yan, Renbin, Yang, Meng, Ybarra, Jason E., Yèche, Christophe, Zakamska, Nadia, Zamora, Olga, Zarrouk, Pauline, Zasowski, Gail, Zhang, Kai, Zhao, Gong-Bo, Zheng, Zheng, Zhou, Zhi-Min, Zhu, Guangtun B., Zoccali, Manuela, Zou, Hu, Blanton, Michael R., Bershady, Matthew A., Abolfathi, Bela, Albareti, Franco D., Prieto, Carlos Allende, Almeida, Andres, Alonso-García, Javier, Anders, Friedrich, Anderson, Scott F., Andrews, Brett, Aquino-Ortíz, Erik, Aragón-Salamanca, Alfonso, Argudo-Fernández, Maria, Armengaud, Eric, Aubourg, Eric, Avila-Reese, Vladimir, Badenes, Carles, Bailey, Stephen, Barger, Kathleen A., Barrera-Ballesteros, Jorge, Bartosz, Curtis, Bates, Dominic, Baumgarten, Falk, Bautista, Julian, Beaton, Rachael, Beers, Timothy C., Belfiore, Francesco, Bender, Chad F., Berlind, Andreas A., Bernardi, Mariangela, Beutler, Florian, Bird, Jonathan C., Bizyaev, Dmitry, Blanc, Guillermo A., Blomqvist, Michael, Bolton, Adam S., Boquien, Médéric, Borissova, Jura, Bosch, Remco van den, Bovy, Jo, Brandt, William N., Brinkmann, Jonathan, Brownstein, Joel R., Bundy, Kevin, Burgasser, Adam J., Burtin, Etienne, Busca, Nicolás G., Cappellari, Michele, Carigi, Maria Leticia Delgado, Carlberg, Joleen K., Rosell, Aurelio Carnero, Carrera, Ricardo, Cherinka, Brian, Cheung, Edmond, Chew, Yilen Gómez Maqueo, Chiappini, Cristina, Choi, Peter Doohyun, Chojnowski, Drew, Chuang, Chia-Hsun, Chung, Haeun, Cirolini, Rafael Fernando, Clerc, Nicolas, Cohen, Roger E., Comparat, Johan, da Costa, Luiz, Cousinou, Marie-Claude, Covey, Kevin, Crane, Jeffrey D., Croft, Rupert A. C., Cruz-Gonzalez, Irene, Cuadra, Daniel Garrido, Cunha, Katia, Damke, Guillermo J., Darling, Jeremy, Davies, Roger, Dawson, Kyle, de la Macorra, Axel, De Lee, Nathan, Delubac, Timothée, Di Mille, Francesco, Diamond-Stanic, Aleks, Cano-Díaz, Mariana, Donor, John, Downes, Juan José, Drory, Niv, Bourboux, Hélion du Mas des, Duckworth, Christopher J., Dwelly, Tom, Dyer, Jamie, Ebelke, Garrett, Eisenstein, Daniel J., Emsellem, Eric, Eracleous, Mike, Escoffier, Stephanie, Evans, Michael L., Fan, Xiaohui, Fernández-Alvar, Emma, Fernandez-Trincado, J. G., Feuillet, Diane K., Finoguenov, Alexis, Fleming, Scott W., Font-Ribera, Andreu, Fredrickson, Alexander, Freischlad, Gordon, Frinchaboy, Peter M., Galbany, Lluís, Garcia-Dias, R., García-Hernández, D. A., Gaulme, Patrick, Geisler, Doug, Gelfand, Joseph D., Gil-Marín, Héctor, Gillespie, Bruce A., Goddard, Daniel, Gonzalez-Perez, Violeta, Grabowski, Kathleen, Green, Paul J., Grier, Catherine J., Gunn, James E., Guo, Hong, Guy, Julien, Hagen, Alex, Hahn, ChangHoon, Hall, Matthew, Harding, Paul, Hasselquist, Sten, Hawley, Suzanne L., Hearty, Fred, Hernández, Jonay I. Gonzalez, Ho, Shirley, Hogg, David W., Holley-Bockelmann, Kelly, Holtzman, Jon A., Holzer, Parker H., Huehnerhoff, Joseph, Hutchinson, Timothy A., Hwang, Ho Seong, Ibarra-Medel, Héctor J., Ilha, Gabriele da Silva, Ivans, Inese I., Ivory, KeShawn, Jackson, Kelly, Jensen, Trey W., Johnson, Jennifer A., Jones, Amy, Jönsson, Henrik, Jullo, Eric, Kamble, Vikrant, Kinemuchi, Karen, Kirkby, David, Kitaura, Francisco-Shu, Klaene, Mark, Knapp, Gillian R., Kneib, Jean-Paul, Kollmeier, Juna A., Lacerna, Ivan, Lane, Richard R., Lang, Dustin, Law, David R., Lazarz, Daniel, Goff, Jean-Marc Le, Liang, Fu-Heng, Li, Cheng, LI, Hongyu, Lima, Marcos, Lin, Lihwai, Lin, Yen-Ting, de Lis, Sara Bertran, Liu, Chao, Lizaola, Miguel Angel C. de Icaza, Long, Dan, Lucatello, Sara, Lundgren, Britt, MacDonald, Nicholas K., Machado, Alice Deconto, MacLeod, Chelsea L., Mahadevan, Suvrath, Maia, Marcio Antonio Geimba, Maiolino, Roberto, Majewski, Steven R., Malanushenko, Elena, Malanushenko, Viktor, Manchado, Arturo, Mao, Shude, Maraston, Claudia, Marques-Chaves, Rui, Masters, Karen L., McBride, Cameron K., McDermid, Richard M., McGrath, Brianne, McGreer, Ian D., Peña, Nicolás Medina, Melendez, Matthew, Merloni, Andrea, Merrifield, Michael R., Meszaros, Szabolcs, Meza, Andres, Minchev, Ivan, Minniti, Dante, Miyaji, Takamitsu, More, Surhud, Mulchaey, John, Müller-Sánchez, Francisco, Muna, Demitri, Munoz, Ricardo R., Myers, Adam D., Nair, Preethi, Nandra, Kirpal, Nascimento, Janaina Correa do, Negrete, Alenka, Ness, Melissa, Newman, Jeffrey A., Nichol, Robert C., Nidever, David L., Nitschelm, Christian, Ntelis, Pierros, O'Connell, Julia E., Oelkers, Ryan J., Oravetz, Audrey, Oravetz, Daniel, Pace, Zach, Padilla, Nelson, Palanque-Delabrouille, Nathalie, Palicio, Pedro Alonso, Pan, Kaike, Parikh, Taniya, Pâris, Isabelle, Park, Changbom, Patten, Alim Y., Peirani, Sebastien, Pellejero-Ibanez, Marcos, Penny, Samantha, Percival, Will J., Perez-Fournon, Ismael, Petitjean, Patrick, Pieri, Matthew M., Pinsonneault, Marc, Pisani, Alice, Poleski, Radosław, Prada, Francisco, Prakash, Abhishek, Queiroz, Anna Bárbara de Andrade, Raddick, M. Jordan, Raichoor, Anand, Rembold, Sandro Barboza, Richstein, Hannah, Riffel, Rogemar A., Riffel, Rogério, Rix, Hans-Walter, Robin, Annie C., Rockosi, Constance M., Rodríguez-Torres, Sergio, Roman-Lopes, A., Román-Zúñiga, Carlos, Rosado, Margarita, Ross, Ashley J., Rossi, Graziano, Ruan, John, Ruggeri, Rossana, Rykoff, Eli S., Salazar-Albornoz, Salvador, Salvato, Mara, Sánchez, Ariel G., Aguado, David Sánchez, Sánchez-Gallego, José R., Santana, Felipe A., Santiago, Basílio Xavier, Sayres, Conor, Schiavon, Ricardo P., Schimoia, Jaderson da Silva, Schlafly, Edward F., Schlegel, David J., Schneider, Donald P., Schultheis, Mathias, Schuster, William J., Schwope, Axel, Seo, Hee-Jong, Shao, Zhengyi, Shen, Shiyin, Shetrone, Matthew, Shull, Michael, Simon, Joshua D., Skinner, Danielle, Skrutskie, M. F., Slosar, Anže, Smith, Verne V., Sobeck, Jennifer S., Sobreira, Flavia, Somers, Garrett, Souto, Diogo, Stark, David V., Stassun, Keivan, Stauffer, Fritz, Steinmetz, Matthias, Storchi-Bergmann, Thaisa, Streblyanska, Alina, Stringfellow, Guy S., Suárez, Genaro, Sun, Jing, Suzuki, Nao, Szigeti, Laszlo, Taghizadeh-Popp, Manuchehr, Tang, Baitian, Tao, Charling, Tayar, Jamie, Tembe, Mita, Teske, Johanna, Thakar, Aniruddha R., Thomas, Daniel, Thompson, Benjamin A., Tinker, Jeremy L., Tissera, Patricia, Tojeiro, Rita, Toledo, Hector Hernandez, de la Torre, Sylvain, Tremonti, Christy, Troup, Nicholas W., Valenzuela, Octavio, Valpuesta, Inma Martinez, Vargas-González, Jaime, Vargas-Magaña, Mariana, Vazquez, Jose Alberto, Villanova, Sandro, Vivek, M., Vogt, Nicole, Wake, David, Walterbos, Rene, Wang, Yuting, Weaver, Benjamin Alan, Weijmans, Anne-Marie, Weinberg, David H., Westfall, Kyle B., Whelan, David G., Wild, Vivienne, Wilson, John, Wood-Vasey, W. M., Wylezalek, Dominika, Xiao, Ting, Yan, Renbin, Yang, Meng, Ybarra, Jason E., Yèche, Christophe, Zakamska, Nadia, Zamora, Olga, Zarrouk, Pauline, Zasowski, Gail, Zhang, Kai, Zhao, Gong-Bo, Zheng, Zheng, Zhou, Zhi-Min, Zhu, Guangtun B., Zoccali, Manuela, and Zou, Hu

Abstract

We describe the Sloan Digital Sky Survey IV (SDSS-IV), a project encompassing three major spectroscopic programs. The Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2) is observing hundreds of thousands of Milky Way stars at high resolution and high signal-to-noise ratio in the near-infrared. The Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey is obtaining spatially-resolved spectroscopy for thousands of nearby galaxies (median redshift of z = 0.03). The extended Baryon Oscillation Spectroscopic Survey (eBOSS) is mapping the galaxy, quasar, and neutral gas distributions between redshifts z = 0.6 and 3.5 to constrain cosmology using baryon acoustic oscillations, redshift space distortions, and the shape of the power spectrum. Within eBOSS, we are conducting two major subprograms: the SPectroscopic IDentification of eROSITA Sources (SPIDERS), investigating X-ray AGN and galaxies in X-ray clusters, and the Time Domain Spectroscopic Survey (TDSS), obtaining spectra of variable sources. All programs use the 2.5-meter Sloan Foundation Telescope at Apache Point Observatory; observations there began in Summer 2014. APOGEE-2 also operates a second near-infrared spectrograph at the 2.5-meter du Pont Telescope at Las Campanas Observatory, with observations beginning in early 2017. Observations at both facilities are scheduled to continue through 2020. In keeping with previous SDSS policy, SDSS-IV provides regularly scheduled public data releases; the first one, Data Release 13, was made available in July 2016., Comment: Published in Astronomical Journal

Published
2017
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529. Discovery of a Very Bright and Intrinsically Very Luminous, Strongly Lensed Ly{\alpha} Emitting Galaxy at z = 2.82 in the BOSS Emission-Line Lens Survey

Author

Marques-Chaves, Rui, Pérez-Fournon, Ismael, Shu, Yiping, Martínez-Navajas, Paloma I., Bolton, Adam S., Kochanek, Christopher S., Oguri, Masamune, Zheng, Zheng, Mao, Shude, Montero-Dorta, Antonio D., Cornachione, Matthew A., Brownstein, Joel R., Marques-Chaves, Rui, Pérez-Fournon, Ismael, Shu, Yiping, Martínez-Navajas, Paloma I., Bolton, Adam S., Kochanek, Christopher S., Oguri, Masamune, Zheng, Zheng, Mao, Shude, Montero-Dorta, Antonio D., Cornachione, Matthew A., and Brownstein, Joel R.

Abstract

We report the discovery of a very bright (r = 20.16), highly magnified, and yet intrinsically very luminous Ly{\alpha} emitter (LAE) at z = 2.82. This system comprises four images in the observer plane with a maximum separation of ~ 6" and it is lensed by a z = 0.55 massive early-type galaxy. It was initially identified in the Baryon Oscillation Spectroscopic Survey (BOSS) Emission-Line Lens Survey for GALaxy-Ly{\alpha} EmitteR sYstems (BELLS GALLERY) survey, and follow-up imaging and spectroscopic observations using the Gran Telescopio Canarias (GTC) and William Herschel Telescope (WHT) confirmed the lensing nature of this system. A lens model using a singular isothermal ellipsoid in an external shear field reproduces quite well the main features of the system, yielding an Einstein radius of 2.95" +/- 0.10", and a total magnification factor for the LAE of 8.8 +/- 0.4. This LAE is one of the brightest and most luminous galaxy-galaxy strong lenses known. We present initial imaging and spectroscopy showing the basic physical and morphological properties of this lensed system., Comment: 6 pages, 3 figures

Published
2017
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530. The alignment between the distribution of satellites and the orientation of their central galaxy

Author

Yang, Xiaohu, Van Den Bosch, Frank C., Mo, H. J., Mao, Shude, Kang, Xi, Weinmann, Simone M., Guo, Yicheng, Jing, Y. P., Yang, Xiaohu, Van Den Bosch, Frank C., Mo, H. J., Mao, Shude, Kang, Xi, Weinmann, Simone M., Guo, Yicheng, and Jing, Y. P.

Abstract

We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation

Published
2017

531. SDSS-IV MaNGA IFS galaxy survey—survey design, execution, and initial data quality

Author

Yan, Renbin, Bundy, Kevin, Law, David R., Bershady, Matthew A., Andrews, Brett, Cherinka, Brian, Diamond-Stanic, Aleksandar M., Drory, Niv, MacDonald, Nicholas, Thomas, Daniel, Wake, David A., Weijmans, Anne-Marie, Westfall, Kyle B., Zhang, Kai, Belfiore, Francesco, Bizyaev, Dmitry, Blanc, Guillermo A., Blanton, Michael R., Brownstein, Joel, Cappellari, Michele, Emsellem, Eric, Fu, Hai, Gaulme, Patrick, Graham, Mark T., Goddard, Daniel, Gunn, James E., Harding, Paul, Jones, Amy, Kinemuchi, Karen, Li, Cheng, Li, Hongyu, Maiolino, Roberto, Mao, Shude, Maraston, Claudia, Masters, Karen, Merrifield, Michael R., Oravetz, Daniel, Pan, Kaike, Parejko, John K., Sanchez, Sebastian F., Schlegel, David, Simmons, Audrey, Thanjavur, Karun, Tinker, Jeremy, Tremonti, Christy, van den Bosch, Remco, and Zheng, Zheng

Subjects
surveys, techniques: imaging spectroscopy, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, galaxies: general, Astrophysics::Galaxy Astrophysics
Abstract

The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy for 10,000 nearby galaxies at a spectral resolution of R ∼ 2000 from 3622 to 10354 Å. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About two-thirds of the sample is covered out to 1.5Re (Primary sample), and one-third of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically the point-spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is ∼70 per 1.4 Å pixel for spectra stacked between 1Re and 1.5Re. Measurements of various galaxy properties from the first-year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.

Published
2016

532. The UV-optical Color Gradients in Star-Forming Galaxies at 0.5

Author

Liu, F. S., Jiang, Dongfei, Guo, Yicheng, Koo, David C., Faber, S. M., Zheng, Xianzhong, Yesuf, Hassen M., Barro, Guillermo, Li, Yao, Li, Dingpeng, Wang, Weichen, Mao, Shude, and Fang, Jerome J.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract

The rest-frame UV-optical (i.e., NUV-B) color index is sensitive to the low-level recent star formation and dust extinction, but it is insensitive to the metallicity. In this Letter, we have measured the rest-frame NUV-B color gradients in ~1400 large ($\rm r_e>0.18^{\prime\prime}$), nearly face-on (b/a>0.5) main-sequence star-forming galaxies (SFGs) between redshift 0.5 and 1.5 in the CANDELS/GOODS-S and UDS fields. With this sample, we study the origin of UV-optical color gradients in the SFGs at z~1 and discuss their link with the buildup of stellar mass. We find that the more massive, centrally compact, and more dust extinguished SFGs tend to have statistically more negative raw color gradients (redder centers) than the less massive, centrally diffuse, and less dusty SFGs. After correcting for dust reddening based on optical-SED fitting, the color gradients in the low-mass ($M_{\ast} 10^{10.5}M_{\odot}$) SFGs still retain shallow negative color gradients. These findings imply that dust reddening is likely the principal cause of negative color gradients in the low-mass SFGs, while both increased central dust reddening and buildup of compact old bulges are likely the origins of negative color gradients in the high-mass SFGs. These findings also imply that at these redshifts the low-mass SFGs buildup their stellar masses in a self-similar way, while the high-mass SFGs grow inside out., 15 pages, 4 figures, accepted for publication in ApJL

Published
2016
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533. The BOSS Emission-Line Lens Survey. III. : Strong Lensing of Ly$��$ Emitters by Individual Galaxies

Author

Shu, Yiping, Bolton, Adam S., Kochanek, Christopher S., Oguri, Masamune, Perez-Fournon, Ismael, Zheng, Zheng, Mao, Shude, Montero-Dorta, Antonio D., Brownstein, Joel R., Marques-Chaves, Rui, and Menard, Brice

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We introduce the Baryon Oscillation Spectroscopic Survey (BOSS) Emission-Line Lens Survey (BELLS) for GALaxy-Ly$��$ EmitteR sYstems (BELLS GALLERY) Survey, which is a Hubble Space Telescope program to image a sample of galaxy-scale strong gravitational lens candidate systems with high-redshift Ly$��$ emitters (LAEs) as the background sources. The goal of the BELLS GALLERY Survey is to illuminate dark substructures in galaxy-scale halos by exploiting the small-scale clumpiness of rest-frame far-UV emission in lensed LAEs, and to thereby constrain the slope and normalization of the substructure-mass function. In this paper, we describe in detail the spectroscopic strong-lens selection technique, which is based on methods adopted in the previous Sloan Lens ACS (SLACS) Survey, BELLS, and SLACS for the Masses Survey. We present the BELLS GALLERY sample of the 21 highest-quality galaxy--LAE candidates selected from $\approx 1.4 \times 10^6$ galaxy spectra in the BOSS of the Sloan Digital Sky Survey III. These systems consist of massive galaxies at redshifts of approximately 0.5 strongly lensing LAEs at redshifts from 2--3. The compact nature of LAEs makes them an ideal probe of dark substructures, with a substructure-mass sensitivity that is unprecedented in other optical strong-lens samples. The magnification effect from lensing will also reveal the structure of LAEs below 100 pc scales, providing a detailed look at the sites of the most concentrated unobscured star formation in the universe. The source code used for candidate selection is available for download as a part of this release., 14 pages, 5 figures, accepted for publication in the ApJ (ApJ, 824, 86). Minor edits to match the ApJ published version

Published
2016
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535. Chemical Abundances and Ages of the Bulge Stars in APOGEE High-velocity Peaks

Author

Zhou, Yingying, primary, Shen, Juntai, additional, Liu, Chao, additional, Li, Zhao-Yu, additional, Mao, Shude, additional, Kunder, Andrea, additional, Rich, R. Michael, additional, Zasowski, G., additional, Fernandez-Trincado, J. G., additional, Majewski, Steven R., additional, Lin, Chien-Cheng, additional, Geisler, Doug, additional, Tang, Baitian, additional, Villanova, S., additional, Roman-Lopes, A., additional, Schultheis, M., additional, Nidever, David L., additional, Meza, Andrés, additional, Pan, Kaike, additional, and Bizyaev, D. V., additional

Published
2017
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537. The Origins of UV–optical Color Gradients in Star-forming Galaxies at z ∼ 2: Predominant Dust Gradients but Negligible sSFR Gradients

Author

Liu, F. S., primary, Jiang, Dongfei, additional, Faber, S. M., additional, Koo, David C., additional, Yesuf, Hassen M., additional, Tacchella, Sandro, additional, Mao, Shude, additional, Wang, Weichen, additional, Guo, Yicheng, additional, Fang, Jerome J., additional, Barro, Guillermo, additional, Zheng, Xianzhong, additional, Jia, Meng, additional, Tong, Wei, additional, Liu, Lu, additional, and Meng, Xianmin, additional

Published
2017
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538. Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe

Author

Blanton, Michael R., primary, Bershady, Matthew A., additional, Abolfathi, Bela, additional, Albareti, Franco D., additional, Prieto, Carlos Allende, additional, Almeida, Andres, additional, Alonso-García, Javier, additional, Anders, Friedrich, additional, Anderson, Scott F., additional, Andrews, Brett, additional, Aquino-Ortíz, Erik, additional, Aragón-Salamanca, Alfonso, additional, Argudo-Fernández, Maria, additional, Armengaud, Eric, additional, Aubourg, Eric, additional, Avila-Reese, Vladimir, additional, Badenes, Carles, additional, Bailey, Stephen, additional, Barger, Kathleen A., additional, Barrera-Ballesteros, Jorge, additional, Bartosz, Curtis, additional, Bates, Dominic, additional, Baumgarten, Falk, additional, Bautista, Julian, additional, Beaton, Rachael, additional, Beers, Timothy C., additional, Belfiore, Francesco, additional, Bender, Chad F., additional, Berlind, Andreas A., additional, Bernardi, Mariangela, additional, Beutler, Florian, additional, Bird, Jonathan C., additional, Bizyaev, Dmitry, additional, Blanc, Guillermo A., additional, Blomqvist, Michael, additional, Bolton, Adam S., additional, Boquien, Médéric, additional, Borissova, Jura, additional, Bosch, Remco van den, additional, Bovy, Jo, additional, Brandt, William N., additional, Brinkmann, Jonathan, additional, Brownstein, Joel R., additional, Bundy, Kevin, additional, Burgasser, Adam J., additional, Burtin, Etienne, additional, Busca, Nicolás G., additional, Cappellari, Michele, additional, Carigi, Maria Leticia Delgado, additional, Carlberg, Joleen K., additional, Rosell, Aurelio Carnero, additional, Carrera, Ricardo, additional, Chanover, Nancy J., additional, Cherinka, Brian, additional, Cheung, Edmond, additional, Chew, Yilen Gómez Maqueo, additional, Chiappini, Cristina, additional, Choi, Peter Doohyun, additional, Chojnowski, Drew, additional, Chuang, Chia-Hsun, additional, Chung, Haeun, additional, Cirolini, Rafael Fernando, additional, Clerc, Nicolas, additional, Cohen, Roger E., additional, Comparat, Johan, additional, Costa, Luiz da, additional, Cousinou, Marie-Claude, additional, Covey, Kevin, additional, Crane, Jeffrey D., additional, Croft, Rupert A. C., additional, Cruz-Gonzalez, Irene, additional, Cuadra, Daniel Garrido, additional, Cunha, Katia, additional, Damke, Guillermo J., additional, Darling, Jeremy, additional, Davies, Roger, additional, Dawson, Kyle, additional, Macorra, Axel de la, additional, Dell’Agli, Flavia, additional, Lee, Nathan De, additional, Delubac, Timothée, additional, Mille, Francesco Di, additional, Diamond-Stanic, Aleks, additional, Cano-Díaz, Mariana, additional, Donor, John, additional, Downes, Juan José, additional, Drory, Niv, additional, Bourboux, Hélion du Mas des, additional, Duckworth, Christopher J., additional, Dwelly, Tom, additional, Dyer, Jamie, additional, Ebelke, Garrett, additional, Eigenbrot, Arthur D., additional, Eisenstein, Daniel J., additional, Emsellem, Eric, additional, Eracleous, Mike, additional, Escoffier, Stephanie, additional, Evans, Michael L., additional, Fan, Xiaohui, additional, Fernández-Alvar, Emma, additional, Fernandez-Trincado, J. G., additional, Feuillet, Diane K., additional, Finoguenov, Alexis, additional, Fleming, Scott W., additional, Font-Ribera, Andreu, additional, Fredrickson, Alexander, additional, Freischlad, Gordon, additional, Frinchaboy, Peter M., additional, Fuentes, Carla E., additional, Galbany, Lluís, additional, Garcia-Dias, R., additional, García-Hernández, D. A., additional, Gaulme, Patrick, additional, Geisler, Doug, additional, Gelfand, Joseph D., additional, Gil-Marín, Héctor, additional, Gillespie, Bruce A., additional, Goddard, Daniel, additional, Gonzalez-Perez, Violeta, additional, Grabowski, Kathleen, additional, Green, Paul J., additional, Grier, Catherine J., additional, Gunn, James E., additional, Guo, Hong, additional, Guy, Julien, additional, Hagen, Alex, additional, Hahn, ChangHoon, additional, Hall, Matthew, additional, Harding, Paul, additional, Hasselquist, Sten, additional, Hawley, Suzanne L., additional, Hearty, Fred, additional, Hernández, Jonay I. Gonzalez, additional, Ho, Shirley, additional, Hogg, David W., additional, Holley-Bockelmann, Kelly, additional, Holtzman, Jon A., additional, Holzer, Parker H., additional, Huehnerhoff, Joseph, additional, Hutchinson, Timothy A., additional, Hwang, Ho Seong, additional, Ibarra-Medel, Héctor J., additional, Ilha, Gabriele da Silva, additional, Ivans, Inese I., additional, Ivory, KeShawn, additional, Jackson, Kelly, additional, Jensen, Trey W., additional, Johnson, Jennifer A., additional, Jones, Amy, additional, Jönsson, Henrik, additional, Jullo, Eric, additional, Kamble, Vikrant, additional, Kinemuchi, Karen, additional, Kirkby, David, additional, Kitaura, Francisco-Shu, additional, Klaene, Mark, additional, Knapp, Gillian R., additional, Kneib, Jean-Paul, additional, Kollmeier, Juna A., additional, Lacerna, Ivan, additional, Lane, Richard R., additional, Lang, Dustin, additional, Law, David R., additional, Lazarz, Daniel, additional, Lee, Youngbae, additional, Goff, Jean-Marc Le, additional, Liang, Fu-Heng, additional, Li, Cheng, additional, Li, Hongyu, additional, Lian, Jianhui, additional, Lima, Marcos, additional, Lin, Lihwai, additional, Lin, Yen-Ting, additional, Lis, Sara Bertran de, additional, Liu, Chao, additional, Lizaola, Miguel Angel C. de Icaza, additional, Long, Dan, additional, Lucatello, Sara, additional, Lundgren, Britt, additional, MacDonald, Nicholas K., additional, Machado, Alice Deconto, additional, MacLeod, Chelsea L., additional, Mahadevan, Suvrath, additional, Maia, Marcio Antonio Geimba, additional, Maiolino, Roberto, additional, Majewski, Steven R., additional, Malanushenko, Elena, additional, Malanushenko, Viktor, additional, Manchado, Arturo, additional, Mao, Shude, additional, Maraston, Claudia, additional, Marques-Chaves, Rui, additional, Masseron, Thomas, additional, Masters, Karen L., additional, McBride, Cameron K., additional, McDermid, Richard M., additional, McGrath, Brianne, additional, McGreer, Ian D., additional, Medina Peña, Nicolás, additional, Melendez, Matthew, additional, Merloni, Andrea, additional, Merrifield, Michael R., additional, Meszaros, Szabolcs, additional, Meza, Andres, additional, Minchev, Ivan, additional, Minniti, Dante, additional, Miyaji, Takamitsu, additional, More, Surhud, additional, Mulchaey, John, additional, Müller-Sánchez, Francisco, additional, Muna, Demitri, additional, Munoz, Ricardo R., additional, Myers, Adam D., additional, Nair, Preethi, additional, Nandra, Kirpal, additional, Nascimento, Janaina Correa do, additional, Negrete, Alenka, additional, Ness, Melissa, additional, Newman, Jeffrey A., additional, Nichol, Robert C., additional, Nidever, David L., additional, Nitschelm, Christian, additional, Ntelis, Pierros, additional, O’Connell, Julia E., additional, Oelkers, Ryan J., additional, Oravetz, Audrey, additional, Oravetz, Daniel, additional, Pace, Zach, additional, Padilla, Nelson, additional, Palanque-Delabrouille, Nathalie, additional, Palicio, Pedro Alonso, additional, Pan, Kaike, additional, Parejko, John K., additional, Parikh, Taniya, additional, Pâris, Isabelle, additional, Park, Changbom, additional, Patten, Alim Y., additional, Peirani, Sebastien, additional, Pellejero-Ibanez, Marcos, additional, Penny, Samantha, additional, Percival, Will J., additional, Perez-Fournon, Ismael, additional, Petitjean, Patrick, additional, Pieri, Matthew M., additional, Pinsonneault, Marc, additional, Pisani, Alice, additional, Poleski, Radosław, additional, Prada, Francisco, additional, Prakash, Abhishek, additional, Queiroz, Anna Bárbara de Andrade, additional, Raddick, M. Jordan, additional, Raichoor, Anand, additional, Rembold, Sandro Barboza, additional, Richstein, Hannah, additional, Riffel, Rogemar A., additional, Riffel, Rogério, additional, Rix, Hans-Walter, additional, Robin, Annie C., additional, Rockosi, Constance M., additional, Rodríguez-Torres, Sergio, additional, Roman-Lopes, A., additional, Román-Zúñiga, Carlos, additional, Rosado, Margarita, additional, Ross, Ashley J., additional, Rossi, Graziano, additional, Ruan, John, additional, Ruggeri, Rossana, additional, Rykoff, Eli S., additional, Salazar-Albornoz, Salvador, additional, Salvato, Mara, additional, Sánchez, Ariel G., additional, Aguado, D. S., additional, Sánchez-Gallego, José R., additional, Santana, Felipe A., additional, Santiago, Basílio Xavier, additional, Sayres, Conor, additional, Schiavon, Ricardo P., additional, Schimoia, Jaderson da Silva, additional, Schlafly, Edward F., additional, Schlegel, David J., additional, Schneider, Donald P., additional, Schultheis, Mathias, additional, Schuster, William J., additional, Schwope, Axel, additional, Seo, Hee-Jong, additional, Shao, Zhengyi, additional, Shen, Shiyin, additional, Shetrone, Matthew, additional, Shull, Michael, additional, Simon, Joshua D., additional, Skinner, Danielle, additional, Skrutskie, M. F., additional, Slosar, Anže, additional, Smith, Verne V., additional, Sobeck, Jennifer S., additional, Sobreira, Flavia, additional, Somers, Garrett, additional, Souto, Diogo, additional, Stark, David V., additional, Stassun, Keivan, additional, Stauffer, Fritz, additional, Steinmetz, Matthias, additional, Storchi-Bergmann, Thaisa, additional, Streblyanska, Alina, additional, Stringfellow, Guy S., additional, Suárez, Genaro, additional, Sun, Jing, additional, Suzuki, Nao, additional, Szigeti, Laszlo, additional, Taghizadeh-Popp, Manuchehr, additional, Tang, Baitian, additional, Tao, Charling, additional, Tayar, Jamie, additional, Tembe, Mita, additional, Teske, Johanna, additional, Thakar, Aniruddha R., additional, Thomas, Daniel, additional, Thompson, Benjamin A., additional, Tinker, Jeremy L., additional, Tissera, Patricia, additional, Tojeiro, Rita, additional, Toledo, Hector Hernandez, additional, Torre, Sylvain de la, additional, Tremonti, Christy, additional, Troup, Nicholas W., additional, Valenzuela, Octavio, additional, Valpuesta, Inma Martinez, additional, Vargas-González, Jaime, additional, Vargas-Magaña, Mariana, additional, Vazquez, Jose Alberto, additional, Villanova, Sandro, additional, Vivek, M., additional, Vogt, Nicole, additional, Wake, David, additional, Walterbos, Rene, additional, Wang, Yuting, additional, Weaver, Benjamin Alan, additional, Weijmans, Anne-Marie, additional, Weinberg, David H., additional, Westfall, Kyle B., additional, Whelan, David G., additional, Wild, Vivienne, additional, Wilson, John, additional, Wood-Vasey, W. M., additional, Wylezalek, Dominika, additional, Xiao, Ting, additional, Yan, Renbin, additional, Yang, Meng, additional, Ybarra, Jason E., additional, Yèche, Christophe, additional, Zakamska, Nadia, additional, Zamora, Olga, additional, Zarrouk, Pauline, additional, Zasowski, Gail, additional, Zhang, Kai, additional, Zhao, Gong-Bo, additional, Zheng, Zheng, additional, Zhou, Xu, additional, Zhou, Zhi-Min, additional, Zhu, Guangtun B., additional, Zoccali, Manuela, additional, and Zou, Hu, additional

Published
2017
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540. The First Data Release of the Beijing-Arizona Sky Survey

Author

Zou, Hu, primary, Zhang, Tianmeng, additional, Zhou, Zhimin, additional, Nie, Jundan, additional, Peng, Xiyan, additional, Zhou, Xu, additional, Jiang, Linhua, additional, Cai, Zheng, additional, Dey, Arjun, additional, Fan, Xiaohui, additional, Fan, Dongwei, additional, Guo, Yucheng, additional, He, Boliang, additional, Jiang, Zhaoji, additional, Lang, Dustin, additional, Lesser, Michael, additional, Li, Zefeng, additional, Ma, Jun, additional, Mao, Shude, additional, McGreer, Ian, additional, Schlegel, David, additional, Shao, Yali, additional, Wang, Jiali, additional, Wang, Shu, additional, Wu, Jin, additional, Wu, Xiaohan, additional, Yang, Qian, additional, and Yue, Minghao, additional

Published
2017
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542. UVI colour gradients of 0.4 < z < 1.4 star-forming main-sequence galaxies in CANDELS: dust extinction and star formation profiles

Author

Wang, Weichen, primary, Faber, S. M., additional, Liu, F. S., additional, Guo, Yicheng, additional, Pacifici, Camilla, additional, Koo, David C., additional, Kassin, Susan A., additional, Mao, Shude, additional, Fang, Jerome J., additional, Chen, Zhu, additional, Koekemoer, Anton M., additional, Kocevski, Dale D., additional, and Ashby, M. L. N., additional

Published
2017
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543. Project Overview of the Beijing–Arizona Sky Survey

Author

Zou, Hu, primary, Zhou, Xu, additional, Fan, Xiaohui, additional, Zhang, Tianmeng, additional, Zhou, Zhimin, additional, Nie, Jundan, additional, Peng, Xiyan, additional, McGreer, Ian, additional, Jiang, Linhua, additional, Dey, Arjun, additional, Fan, Dongwei, additional, He, Boliang, additional, Jiang, Zhaoji, additional, Lang, Dustin, additional, Lesser, Michael, additional, Ma, Jun, additional, Mao, Shude, additional, Schlegel, David, additional, and Wang, Jiali, additional

Published
2017
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545. Discovery of a Very Bright and Intrinsically Very Luminous, Strongly Lensed Ly α Emitting Galaxy at z = 2.82 in the BOSS Emission-Line Lens Survey

Author

Marques-Chaves, Rui, primary, Pérez-Fournon, Ismael, additional, Shu, Yiping, additional, Martínez-Navajas, Paloma I., additional, Bolton, Adam S., additional, Kochanek, Christopher S., additional, Oguri, Masamune, additional, Zheng, Zheng, additional, Mao, Shude, additional, Montero-Dorta, Antonio D., additional, Cornachione, Matthew A., additional, and Brownstein, Joel R., additional

Published
2017
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546. THE BOSS EMISSION-LINE LENS SURVEY. IV. SMOOTH LENS MODELS FOR THE BELLS GALLERY SAMPLE

Author

Shu, Yiping, primary, Bolton, Adam S., additional, Mao, Shude, additional, Kochanek, Christopher S., additional, Pérez-Fournon, Ismael, additional, Oguri, Masamune, additional, Montero-Dorta, Antonio D., additional, Cornachione, Matthew A., additional, Marques-Chaves, Rui, additional, Zheng, Zheng, additional, Brownstein, Joel R., additional, and Ménard, Brice, additional

Published
2016
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547. Combining time delays and image positions for quadruple lenses: a moment approach

Author

Witt, Hans and Mao, Shude

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Computer Science::Databases, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Time delays in gravitational lenses can be used to determine the Hubble constant and the lens potential. In future surveys, many gravitational lenses can be discovered, and their time delays and image positions can in principle be measured. Using an elliptical power-law potential, we show that combinations of image positions and time delays for quadruple lenses yield simple analytical expressions that are connected with observable quantities. These relations can be used to obtain the approximate axis ratio q, the Einstein radius and the slope. We apply this method to RX J1131-1231, and show that our analytical results match the full numerical determinations approximately. Our approach can quickly determine rough values of lens parameters, which can then be used as initial guesses for further refinement through numerical modelling and may be useful for automated lens search in large surveys., 9 pages, one figure, MNRAS, in press

Published
2015

548. Overview of the SDSS-IV MaNGA survey: mapping nearby galaxies at Apache Point Observatory

Author

Bundy, Kevin, Bershady, Matthew A., Law, David R., Yan, Renbin, Drory, Niv, MacDonald, Nicholas, Wake, David A., Cherinka, Brian, Weijmans, Anne-Marie, Thomas, Daniel, Tremonti, Christy, Masters, Karen, Coccato, Lodovico, Diamond-Stanic, Aleksandar M., Avila-Reese, Vladimir, Badenes, Carles, Belfiore, Francesco, Bizyaev, Dmitry, Blanc, Guillermo A., Bland-Hawthorn, Joss, Blanton, Michael R., Brownstein, Joel R., Byler, Nell, Cappellari, Michele, Conroy, Charlie, Dutton, Aaron A., Emsellem, Eric, Etherington, James, Frinchaboy, Peter M., Fu, Hai, Gunn, James E., Harding, Paul, Johnston, Evelyn J., Kauffmann, Guinevere, Kinemuchi, Karen, Klaene, Mark A., Knapen, Johan H., Leauthaud, Alexie, Li, Cheng, Lin, Lihwai, Maiolino, Roberto, Malanushenko, Viktor, Malanushenko, Elena, Mao, Shude, Maraston, Claudia, McDermid, Richard M., Merrifield, Michael R., Nichol, Robert C., Oravetz, Daniel, Pan, Kaike, Parejko, John K., Sanchez, Sebastian F., Schlegel, David, Simmons, Audrey, Steele, Oliver, Steinmetz, Matthias, Thanjavur, Karun, Thompson, Benjamin A., Tinker, Jeremy L., van den Bosch, Remco C. E., Westfall, Kyle B., Wilkinson, David, Wright, Shelley, Xiao, Ting, and Zhang, Kai

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present an overview of a new integral field spectroscopic survey called MaNGA (Mapping Nearby Galaxies at Apache Point Observatory), one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV) that began on 2014 July 1. MaNGA will investigate the internal kinematic structure and composition of gas and stars in an unprecedented sample of 10,000 nearby galaxies. We summarize essential characteristics of the instrument and survey design in the context of MaNGA's key science goals and present prototype observations to demonstrate MaNGA's scientific potential. MaNGA employs dithered observations with 17 fiber-bundle integral field units that vary in diameter from 12'' (19 fibers) to 32'' (127 fibers). Two dual-channel spectrographs provide simultaneous wavelength coverage over 3600-10300 Å at R ~ 2000. With a typical integration time of 3 hr, MaNGA reaches a target r-band signal-to-noise ratio of 4-8 (Å–1 per 2'' fiber) at 23 AB mag arcsec–2, which is typical for the outskirts of MaNGA galaxies. Targets are selected with M * 109 M ☉ using SDSS-I redshifts and i-band luminosity to achieve uniform radial coverage in terms of the effective radius, an approximately flat distribution in stellar mass, and a sample spanning a wide range of environments. Analysis of our prototype observations demonstrates MaNGA's ability to probe gas ionization, shed light on recent star formation and quenching, enable dynamical modeling, decompose constituent components, and map the composition of stellar populations. MaNGA's spatially resolved spectra will enable an unprecedented study of the astrophysics of nearby galaxies in the coming 6 yr.

Published
2014

549. Orbit properties of massive prolate galaxies in the Illustris simulation.

Author

Wang, Yougang, Mao, Shude, Li, Hongyu, Xu, Dandan, Chen, Xuelei, and Springel, Volker

Subjects
*GALAXIES, *ORBITS (Astronomy), *HYDRODYNAMICS, *BARYONS, *SCHWARZSCHILD black holes
Abstract

We explore orbit properties of 35 prolate-triaxial galaxies selected from the Illustris cosmological hydrodynamic simulation. We present a detailed study of their orbit families, and also analyse relations between the relative abundance of the orbit families and the spin parameter, triaxiality, the ratio of the angular momentum, and the baryon fraction. We find that box orbits dominate the orbit structure for most prolate-triaxial galaxies, especially in the central region. The fraction of irregular orbits in the prolate-triaxial galaxies is small, and it increases with galaxy radius. Both the x -tube and z -tube orbits are important in prolate-triaxial galaxies, especially in the outer regions. The fraction of box orbits for prolate-triaxial galaxies (0.7 < T < 1) decreases with the triaxiality of the stars, while the fraction of x -tube orbits increases with the triaxiality for a given axis ratio. The fraction of box orbits increases and the fractions of x -tube and z -tube orbits weakly decrease with increasing baryon fraction. These results help to understand the structure of prolate-triaxial galaxies and provide cross-checks for constructing dynamical models of prolate-triaxial galaxies by using the Schwarzschild or the made-to-measure methods. [ABSTRACT FROM AUTHOR]

Published
2019
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550. SDSS-IV MaNGA: pattern speeds of barred galaxies.

Author

Guo, Rui, Mao, Shude, Athanassoula, E, Li, Hongyu, Ge, Junqiang, Long, R J, Merrifield, Michael, and Masters, Karen

Subjects
*BARRED galaxies, *GALACTIC dynamics, *ASTRONOMICAL photometry, *STELLAR populations, *STAR formation, *GALACTIC evolution
Abstract

The MaNGA project has obtained integral field unit (IFU) data for several thousand nearby galaxies, including barred galaxies. With the two-dimensional spectral and kinematic information provided by IFUs, we can measure the pattern speed of a barred galaxy, which determines the bar dynamics. We apply the non-parametric method proposed by Tremaine & Weinberg to estimate the bar pattern speed for 53 barred galaxies, making this the largest sample studied so far in this way. Our sample is selected from the MaNGA first public data release as part of SDSS Data Release 13 according mainly to the axial ratio and position angle difference between the bar and disc, while kinematic data are from the later SDSS Data Release 14. We have used both the photometric position angle from the photometric image and the kinematic position angle from the stellar velocity map to derive the pattern speed. Combining three independent bar length measurements and the circular velocity from Jeans anisotropic modelling (JAM), we also determine the dimensionless ratio |$\cal {R}$| of the corotation radius to the bar length. We find that the galaxy's position angle is the main uncertainty in determining the bar pattern speed. The kinematic position angle leads to fewer ultrafast bars than the photometric position angle, and this could be due to the method of measuring the kinematic position angle. We study the dependence of |$\cal {R}$| values on galaxy properties such as the dark matter fraction from JAM modelling and the stellar age and metallicity from stellar population synthesis. A positive correlation between the bar length and bar strength is found: the longer the bar, the stronger the bar. However, no other significant correlations are found. This may result from errors in deriving the |$\cal {R}$| values or from the complex formation and slowdown processes of galactic bars. [ABSTRACT FROM AUTHOR]

Published
2019
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