TY - JOUR AB - The quantum anomalous Hall (QAH) effect combines topology and magnetism to produce precisely quantized Hall resistance at zero magnetic field. We report the observation of a QAH effect in twisted bilayer graphene aligned to hexagonal boron nitride. The effect is driven by intrinsic strong interactions, which polarize the electrons into a single spin- and valley-resolved moiré miniband with Chern number C = 1. In contrast to magnetically doped systems, the measured transport energy gap is larger than the Curie temperature for magnetic ordering, and quantization to within 0.1% of the von Klitzing constant persists to temperatures of several kelvin at zero magnetic field. Electrical currents as small as 1 nanoampere controllably switch the magnetic order between states of opposite polarization, forming an electrically rewritable magnetic memory. AU - Serlin, M. AU - Tschirhart, C. L. AU - Polshyn, Hryhoriy AU - Zhang, Y. AU - Zhu, J. AU - Watanabe, K. AU - Taniguchi, T. AU - Balents, L. AU - Young, A. F. ID - 10619 IS - 6480 JF - Science KW - multidisciplinary SN - 0036-8075 TI - Intrinsic quantized anomalous Hall effect in a moiré heterostructure VL - 367 ER - TY - CONF AB - Twisted bilayer graphene (tBLG) near the flat band condition is a versatile new platform for the study of correlated physics in 2D. Resistive states have been observed at several commensurate fillings of the flat miniband, along with superconducting states near half filling. To better understand the electronic structure of this system, we study electronic transport of graphite gated superconducting tBLG devices in the normal regime. At high magnetic fields, we observe full lifting of the spin and valley degeneracy. The transitions in the splitting of this four-fold degeneracy as a function of carrier density indicate Landau level (LL) crossings, which tilted field measurements show occur between LLs with different valley polarization. Similar LL structure measured in two devices, one with twist angle θ=1.08° at ambient pressure and one at θ=1.27° and 1.33GPa, suggests that the dimensionless combination of twist angle and interlayer coupling controls the relevant details of the band structure. In addition, we find that the temperature dependence of the resistance at B=0 shows linear growth at several hundred Ohm/K in a broad range of temperatures. We discuss the implications for modeling the scattering processes in this system. AU - Polshyn, Hryhoriy AU - Zhang, Yuxuan AU - Yankowitz, Matthew AU - Chen, Shaowen AU - Taniguchi, Takashi AU - Watanabe, Kenji AU - Graf, David E. AU - Dean, Cory R. AU - Young, Andrea ID - 10724 IS - 2 SN - 0003-0503 T2 - APS March Meeting 2019 TI - Normal state transport in superconducting twisted bilayer graphene VL - 64 ER - TY - CONF AB - Bilayer graphene, rotationally faulted to ~1.1 degree misalignment, has recently been shown to host superconducting and resistive states associated with the formation of a flat electronic band. While numerous theories exist for the origins of both states, direct validation of these theories remains an outstanding experimental problem. Here, we focus on the resistive states occurring at commensurate filling (1/2, 1/4, and 3/4) of the two lowest superlattice bands. We test theoretical proposals that these states arise due to broken spin—and/or valley—symmetry by performing direct magnetic imaging with nanoscale SQUID-on-tip microscopy. This technique provides single-spin resolved magnetometry on sub-100nm length scales. I will present imaging data from our 4.2K nSOT microscope on graphite-gated twisted bilayers near the flat band condition and discuss the implications for the physics of the commensurate resistive states. AU - Serlin, Marec AU - Tschirhart, Charles AU - Polshyn, Hryhoriy AU - Zhu, Jiacheng AU - Huber, Martin E. AU - Young, Andrea ID - 10722 IS - 2 SN - 0003-0503 T2 - APS March Meeting 2019 TI - Direct Imaging of magnetic structure in twisted bilayer graphene with scanning nanoSQUID-On-Tip microscopy VL - 64 ER - TY - CONF AB - Bilayer graphene with ~ 1.1 degrees twist mismatch between the layers hosts a low energy flat band in which the Coulomb interaction is large relative to the bandwidth, promoting correlated insulating states at half band filling, and superconducting (SC) phases with dome-like structure neighboring correlated insulating states. Here we show measurements of a dual-graphite-gated twisted bilayer graphene device, which minimizes charge inhomogeneity. We observe new correlated phases, including for the first time a SC pocket near half-filling of the electron-doped band and resistive states at quarter-filling of both bands that emerge in a magnetic field. Changing the layer polarization with vertical electric field reveals an unexpected competition between SC and correlated insulator phases, which we interpret to result from differences in disorder of each graphene layer and underscores the spatial inhomogeneity like twist angle as a significant source of disorder in these devices [1]. AU - Chen, Shaowen AU - Yankowitz, Matthew AU - Polshyn, Hryhoriy AU - Watanabe, Kenji AU - Taniguchi, Takashi AU - Graf, David E. AU - Young, Andrea AU - Dean, Cory R. ID - 10725 IS - 2 SN - 0003-0503 T2 - APS March Meeting 2019 TI - Correlated insulating and superconducting phases in twisted bilayer graphene VL - 64 ER - TY - CONF AB - In monolayer graphene, the interplay of electronic correlations with the internal spin- and valley- degrees of freedom leads to a complex phase diagram of isospin symmetry breaking at high magnetic fields. Recently, Wei et al. (Science (2018)) demonstrated that spin waves can be electrically generated and detected in graphene heterojunctions, allowing direct experiment access to the spin degree of freedom. Here, we apply this technique to high quality graphite-gated graphene devices showing robust fractional quantum Hall phases and isospin phase transitions. We use an edgeless Corbino geometry to eliminate the contributions of edge states to the spin-wave mediated nonlocal voltage, allowing unambiguous identification of spin wave transport signatures. Our data reveal two phases within the ν = 1 plateau. For exactly ν=1, charge is localized but spin waves propagate freely while small carrier doping completely quenches the low-energy spin-wave transport, even as those charges remain localized. We identify this new phase as a spin textured electron solid. We also find that spin-wave transport is modulated by phase transitions in the valley order that preserve spin polarization, suggesting that this technique is sensitive to both spin and valley order. AU - Zhou, Haoxin AU - Polshyn, Hryhoriy AU - Tanaguchi, Takashi AU - Watanabe, Kenji AU - Young, Andrea ID - 10723 IS - 2 SN - 0003-0503 T2 - APS March Meeting 2019 TI - Spin wave transport through electron solids and fractional quantum Hall liquids in graphene VL - 64 ER - TY - CONF AB - This report presents the results of a friendly competition for formal verification of continuous and hybrid systems with piecewise constant dynamics. The friendly competition took place as part of the workshop Applied Verification for Continuous and Hybrid Systems (ARCH) in 2019. In this third edition, six tools have been applied to solve five different benchmark problems in the category for piecewise constant dynamics: BACH, Lyse, Hy- COMP, PHAVer/SX, PHAVerLite, and VeriSiMPL. Compared to last year, a new tool has participated (HyCOMP) and PHAVerLite has replaced PHAVer-lite. The result is a snap- shot of the current landscape of tools and the types of benchmarks they are particularly suited for. Due to the diversity of problems, we are not ranking tools, yet the presented results probably provide the most complete assessment of tools for the safety verification of continuous and hybrid systems with piecewise constant dynamics up to this date. AU - Frehse, Goran AU - Abate, Alessandro AU - Adzkiya, Dieky AU - Becchi, Anna AU - Bu, Lei AU - Cimatti, Alessandro AU - Giacobbe, Mirco AU - Griggio, Alberto AU - Mover, Sergio AU - Mufid, Muhammad Syifa'ul AU - Riouak, Idriss AU - Tonetta, Stefano AU - Zaffanella, Enea ED - Frehse, Goran ED - Althoff, Matthias ID - 10877 SN - 2398-7340 T2 - ARCH19. 6th International Workshop on Applied Verification of Continuous and Hybrid Systems TI - ARCH-COMP19 Category Report: Hybrid systems with piecewise constant dynamics VL - 61 ER - TY - JOUR AB - Many adult tissues contain postmitotic cells as old as the host organism. The only organelle that does not turn over in these cells is the nucleus, and its maintenance represents a formidable challenge, as it harbors regulatory proteins that persist throughout adulthood. Here we developed strategies to visualize two classes of such long-lived proteins, histones and nucleoporins, to understand the function of protein longevity in nuclear maintenance. Genome-wide mapping of histones revealed specific enrichment of long-lived variants at silent gene loci. Interestingly, nuclear pores are maintained by piecemeal replacement of subunits, resulting in mosaic complexes composed of polypeptides with vastly different ages. In contrast, nondividing quiescent cells remove old nuclear pores in an ESCRT-dependent manner. Our findings reveal distinct molecular strategies of nuclear maintenance, linking lifelong protein persistence to gene regulation and nuclear integrity. AU - Toyama, Brandon H. AU - Arrojo e Drigo, Rafael AU - Lev-Ram, Varda AU - Ramachandra, Ranjan AU - Deerinck, Thomas J. AU - Lechene, Claude AU - Ellisman, Mark H. AU - HETZER, Martin W ID - 11061 IS - 2 JF - Journal of Cell Biology KW - Cell Biology SN - 0021-9525 TI - Visualization of long-lived proteins reveals age mosaicism within nuclei of postmitotic cells VL - 218 ER - TY - JOUR AB - Most neurons are not replaced during an animal’s lifetime. This nondividing state is characterized by extreme longevity and age-dependent decline of key regulatory proteins. To study the lifespans of cells and proteins in adult tissues, we combined isotope labeling of mice with a hybrid imaging method (MIMS-EM). Using 15N mapping, we show that liver and pancreas are composed of cells with vastly different ages, many as old as the animal. Strikingly, we also found that a subset of fibroblasts and endothelial cells, both known for their replicative potential, are characterized by the absence of cell division during adulthood. In addition, we show that the primary cilia of beta cells and neurons contains different structural regions with vastly different lifespans. Based on these results, we propose that age mosaicism across multiple scales is a fundamental principle of adult tissue, cell, and protein complex organization. AU - Arrojo e Drigo, Rafael AU - Lev-Ram, Varda AU - Tyagi, Swati AU - Ramachandra, Ranjan AU - Deerinck, Thomas AU - Bushong, Eric AU - Phan, Sebastien AU - Orphan, Victoria AU - Lechene, Claude AU - Ellisman, Mark H. AU - HETZER, Martin W ID - 11062 IS - 2 JF - Cell Metabolism KW - Cell Biology KW - Molecular Biology KW - Physiology SN - 1550-4131 TI - Age mosaicism across multiple scales in adult tissues VL - 30 ER - TY - JOUR AB - Deep optical spectroscopic surveys of galaxies provide a unique opportunity to investigate rest-frame ultra-violet (UV) emission line properties of galaxies at z ∼ 2 − 4.5. Here we combine VLT/MUSE Guaranteed Time Observations of the Hubble Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other publicly available data from VLT/VIMOS and VLT/FORS2 to construct a catalogue of He II λ1640 emitters at z ≳ 2. The deepest areas of our MUSE pointings reach a 3σ line flux limit of 3.1 × 10−19 erg s−1 cm−2. After discarding broad-line active galactic nuclei, we find 13 He II λ1640 detections from MUSE with a median MUV = −20.1 and 21 tentative He II λ1640 detections from other public surveys. Excluding Lyα, all except two galaxies in our sample show at least one other rest-UV emission line, with C III] λ1907, λ1909 being the most prominent. We use multi-wavelength data available in the Hubble legacy fields to derive basic galaxy properties of our sample through spectral energy distribution fitting techniques. Taking advantage of the high-quality spectra obtained by MUSE (∼10 − 30 h of exposure time per pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics of the He II λ1640 emitters. Line ratios of our sample can be reproduced by moderately sub-solar photo-ionisation models, however, we find that including effects of binary stars lead to degeneracies in most free parameters. Even after considering extra ionising photons produced by extreme sub-solar metallicity binary stellar models, photo-ionisation models are unable to reproduce rest-frame He II λ1640 equivalent widths (∼0.2 − 10 Å), thus additional mechanisms are necessary in models to match the observed He II λ1640 properties. AU - Nanayakkara, Themiya AU - Brinchmann, Jarle AU - Boogaard, Leindert AU - Bouwens, Rychard AU - Cantalupo, Sebastiano AU - Feltre, Anna AU - Kollatschny, Wolfram AU - Marino, Raffaella Anna AU - Maseda, Michael AU - Matthee, Jorryt J AU - Paalvast, Mieke AU - Richard, Johan AU - Verhamme, Anne ID - 11499 JF - Astronomy & Astrophysics KW - Space and Planetary Science KW - Astronomy and Astrophysics KW - galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift SN - 0004-6361 TI - Exploring He II λ1640 emission line properties at z ∼2−4 VL - 648 ER - TY - JOUR AB - Contact. This paper presents the results obtained with the Multi-Unit Spectroscopic Explorer (MUSE) at the ESO Very Large Telescope on the faint end of the Lyman-alpha luminosity function (LF) based on deep observations of four lensing clusters. The goal of our project is to set strong constraints on the relative contribution of the Lyman-alpha emitter (LAE) population to cosmic reionization. Aims. The precise aim of the present study is to further constrain the abundance of LAEs by taking advantage of the magnification provided by lensing clusters to build a blindly selected sample of galaxies which is less biased than current blank field samples in redshift and luminosity. By construction, this sample of LAEs is complementary to those built from deep blank fields, whether observed by MUSE or by other facilities, and makes it possible to determine the shape of the LF at fainter levels, as well as its evolution with redshift. Methods. We selected a sample of 156 LAEs with redshifts between 2.9 ≤ z ≤ 6.7 and magnification-corrected luminosities in the range 39 ≲ log LLyα [erg s−1] ≲43. To properly take into account the individual differences in detection conditions between the LAEs when computing the LF, including lensing configurations, and spatial and spectral morphologies, the non-parametric 1/Vmax method was adopted. The price to pay to benefit from magnification is a reduction of the effective volume of the survey, together with a more complex analysis procedure to properly determine the effective volume Vmax for each galaxy. In this paper we present a complete procedure for the determination of the LF based on IFU detections in lensing clusters. This procedure, including some new methods for masking, effective volume integration and (individual) completeness determinations, has been fully automated when possible, and it can be easily generalized to the analysis of IFU observations in blank fields. Results. As a result of this analysis, the Lyman-alpha LF has been obtained in four different redshift bins: 2.9 <  z <  6, 7, 2.9 <  z <  4.0, 4.0 <  z <  5.0, and 5.0 <  z <  6.7 with constraints down to log LLyα = 40.5. From our data only, no significant evolution of LF mean slope can be found. When performing a Schechter analysis also including data from the literature to complete the present sample towards the brightest luminosities, a steep faint end slope was measured varying from α = −1.69−0.08+0.08 to α = −1.87−0.12+0.12 between the lowest and the highest redshift bins. Conclusions. The contribution of the LAE population to the star formation rate density at z ∼ 6 is ≲50% depending on the luminosity limit considered, which is of the same order as the Lyman-break galaxy (LBG) contribution. The evolution of the LAE contribution with redshift depends on the assumed escape fraction of Lyman-alpha photons, and appears to slightly increase with increasing redshift when this fraction is conservatively set to one. Depending on the intersection between the LAE/LBG populations, the contribution of the observed galaxies to the ionizing flux may suffice to keep the universe ionized at z ∼ 6. AU - de La Vieuville, G. AU - Bina, D. AU - Pello, R. AU - Mahler, G. AU - Richard, J. AU - Drake, A. B. AU - Herenz, E. C. AU - Bauer, F. E. AU - Clément, B. AU - Lagattuta, D. AU - Laporte, N. AU - Martinez, J. AU - Patrício, V. AU - Wisotzki, L. AU - Zabl, J. AU - Bouwens, R. J. AU - Contini, T. AU - Garel, T. AU - Guiderdoni, B. AU - Marino, R. A. AU - Maseda, M. V. AU - Matthee, Jorryt J AU - Schaye, J. AU - Soucail, G. ID - 11505 JF - Astronomy & Astrophysics KW - Space and Planetary Science KW - Astronomy and Astrophysics KW - gravitational lensing: strong / galaxies: high-redshift / dark ages KW - reionization KW - first stars / galaxies: clusters: general / galaxies: luminosity function KW - mass function SN - 0004-6361 TI - Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE VL - 628 ER - TY - JOUR AB - Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies. While it originates from many physical processes, for star-forming galaxies the intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star formation rate (SFR) indicator. However, its resonant nature and susceptibility to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs) at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and we show that it constrains a well-defined anti-correlation between ionisation efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0 are easy measurable quantities at high redshift, thus making our relation a practical tool to estimate intrinsic Lyα and LyC luminosities under well controlled and simple assumptions. Our results allow observed Lyα luminosities to be used to compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs. We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6 to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1 and that our calibration might be even applicable for the most luminous LAEs within the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1] = 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily tested with future observations with JWST which can obtain Hα and Hβ measurements for high-redshift LAEs. AU - Sobral, David AU - Matthee, Jorryt J ID - 11507 JF - Astronomy & Astrophysics KW - Space and Planetary Science KW - Astronomy and Astrophysics KW - galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies: evolution / galaxies: formation / galaxies: ISM SN - 0004-6361 TI - Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator VL - 623 ER - TY - JOUR AB - We discuss the nature and physical properties of gas-mass selected galaxies in the ALMA spectroscopic survey (ASPECS) of the Hubble Ultra Deep Field (HUDF). We capitalize on the deep optical integral-field spectroscopy from the Multi Unit Spectroscopic Explorer (MUSE) HUDF Survey and multiwavelength data to uniquely associate all 16 line emitters, detected in the ALMA data without preselection, with rotational transitions of carbon monoxide (CO). We identify 10 as CO(2–1) at 1 < z < 2, 5 as CO(3–2) at 2 < z < 3, and 1 as CO(4–3) at z = 3.6. Using the MUSE data as a prior, we identify two additional CO(2–1) emitters, increasing the total sample size to 18. We infer metallicities consistent with (super-)solar for the CO-detected galaxies at z ≤ 1.5, motivating our choice of a Galactic conversion factor between CO luminosity and molecular gas mass for these galaxies. Using deep Chandra imaging of the HUDF, we determine an X-ray AGN fraction of 20% and 60% among the CO emitters at z ∼ 1.4 and z ∼ 2.6, respectively. Being a CO-flux-limited survey, ASPECS-LP detects molecular gas in galaxies on, above, and below the main sequence (MS) at z ∼ 1.4. For stellar masses ≥1010 (1010.5) ${M}_{\odot }$, we detect about 40% (50%) of all galaxies in the HUDF at 1 < z < 2 (2 < z < 3). The combination of ALMA and MUSE integral-field spectroscopy thus enables an unprecedented view of MS galaxies during the peak of galaxy formation. AU - Boogaard, Leindert A. AU - Decarli, Roberto AU - González-López, Jorge AU - van der Werf, Paul AU - Walter, Fabian AU - Bouwens, Rychard AU - Aravena, Manuel AU - Carilli, Chris AU - Bauer, Franz Erik AU - Brinchmann, Jarle AU - Contini, Thierry AU - Cox, Pierre AU - da Cunha, Elisabete AU - Daddi, Emanuele AU - Díaz-Santos, Tanio AU - Hodge, Jacqueline AU - Inami, Hanae AU - Ivison, Rob AU - Maseda, Michael AU - Matthee, Jorryt J AU - Oesch, Pascal AU - Popping, Gergö AU - Riechers, Dominik AU - Schaye, Joop AU - Schouws, Sander AU - Smail, Ian AU - Weiss, Axel AU - Wisotzki, Lutz AU - Bacon, Roland AU - Cortes, Paulo C. AU - Rix, Hans-Walter AU - Somerville, Rachel S. AU - Swinbank, Mark AU - Wagg, Jeff ID - 11514 IS - 2 JF - The Astrophysical Journal KW - Space and Planetary Science KW - Astronomy and Astrophysics SN - 0004-637X TI - The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy VL - 882 ER - TY - JOUR AB - The well-known quasar SDSS J095253.83+011421.9 (J0952+0114) at z = 3.02 has one of the most peculiar spectra discovered so far, showing the presence of narrow Lyα and broad metal emission lines. Although recent studies have suggested that a proximate damped Lyα absorption (PDLA) system causes this peculiar spectrum, the origin of the gas associated with the PDLA is unknown. Here we report the results of observations with the Multi Unit Spectroscopic Explorer (MUSE) that reveal a new giant (≈100 physical kpc) Lyα nebula. The detailed analysis of the Lyα velocity, velocity dispersion, and surface brightness profiles suggests that the J0952+0114 Lyα nebula shares similar properties with other QSO nebulae previously detected with MUSE, implying that the PDLA in J0952+0144 is covering only a small fraction of the solid angle of the QSO emission. We also detected bright and spectrally narrow C iv λ1550 and He ii λ1640 extended emission around J0952+0114 with velocity centroids similar to the peak of the extended and central narrow Lyα emission. The presence of a peculiarly bright, unresolved, and relatively broad He ii λ1640 emission in the central region at exactly the same PDLA redshift hints at the possibility that the PDLA originates in a clumpy outflow with a bulk velocity of about 500 km s−1. The smaller velocity dispersion of the large-scale Lyα emission suggests that the high-speed outflow is confined to the central region. Lastly, the derived spatially resolved He ii/Lyα and C iv/Lyα maps show a positive gradient with the distance to the QSO, hinting at a non-homogeneous distribution of the ionization parameter. AU - Marino, Raffaella Anna AU - Cantalupo, Sebastiano AU - Pezzulli, Gabriele AU - Lilly, Simon J. AU - Gallego, Sofia AU - Mackenzie, Ruari AU - Matthee, Jorryt J AU - Brinchmann, Jarle AU - Bouché, Nicolas AU - Feltre, Anna AU - Muzahid, Sowgat AU - Schroetter, Ilane AU - Johnson, Sean D. AU - Nanayakkara, Themiya ID - 11516 IS - 1 JF - The Astrophysical Journal KW - Space and Planetary Science KW - Astronomy and Astrophysics SN - 0004-637X TI - A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE VL - 880 ER - TY - JOUR AB - We present new deep ALMA and Hubble Space Telescope (HST)/WFC3 observations of MASOSA and VR7, two luminous Lyα emitters (LAEs) at z = 6.5, for which the UV continuum levels differ by a factor of four. No IR dust continuum emission is detected in either, indicating little amounts of obscured star formation and/or high dust temperatures. MASOSA, with a UV luminosity M1500 = −20.9, compact size, and very high Lyα ${\mathrm{EW}}_{0}\approx 145\,\mathring{\rm A} $, is undetected in [C ii] to a limit of L[C ii] < 2.2 × 107 L⊙, implying a metallicity Z ≲ 0.07 Z⊙. Intriguingly, our HST data indicate a red UV slope β = −1.1 ± 0.7, at odds with the low dust content. VR7, which is a bright (M1500 = −22.4) galaxy with moderate color (β = −1.4 ± 0.3) and Lyα EW0 = 34 Å, is clearly detected in [C ii] emission (S/N = 15). VR7's rest-frame UV morphology can be described by two components separated by ≈1.5 kpc and is globally more compact than the [C ii] emission. The global [C ii]/UV ratio indicates Z ≈ 0.2 Z⊙, but there are large variations in the UV/[C ii] ratio on kiloparsec scales. We also identify diffuse, possibly outflowing, [C ii]-emitting gas at ≈100 km s−1 with respect to the peak. VR7 appears to be assembling its components at a slightly more evolved stage than other luminous LAEs, with outflows already shaping its direct environment at z ∼ 7. Our results further indicate that the global [C ii]−UV relation steepens at SFR < 30 M⊙ yr−1, naturally explaining why the [C ii]/UV ratio is anticorrelated with Lyα EW in many, but not all, observed LAEs. AU - Matthee, Jorryt J AU - Sobral, D. AU - Boogaard, L. A. AU - Röttgering, H. AU - Vallini, L. AU - Ferrara, A. AU - Paulino-Afonso, A. AU - Boone, F. AU - Schaerer, D. AU - Mobasher, B. ID - 11515 IS - 2 JF - The Astrophysical Journal KW - Space and Planetary Science KW - Astronomy and Astrophysics SN - 0004-637X TI - Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization VL - 881 ER - TY - JOUR AB - To understand star formation in galaxies, we investigate the star formation rate (SFR) surface density (ΣSFR) profiles for galaxies, based on a well-defined sample of 976 star-forming MaNGA galaxies. We find that the typical ΣSFR profiles within 1.5Re of normal SF galaxies can be well described by an exponential function for different stellar mass intervals, while the sSFR profile shows positive gradients, especially for more massive SF galaxies. This is due to the more pronounced central cores or bulges rather than the onset of a `quenching' process. While galaxies that lie significantly above (or below) the star formation main sequence (SFMS) show overall an elevation (or suppression) of ΣSFR at all radii, this central elevation (or suppression) is more pronounced in more massive galaxies. The degree of central enhancement and suppression is quite symmetric, suggesting that both the elevation and suppression of star formation are following the same physical processes. Furthermore, we find that the dispersion in ΣSFR within and across the population is found to be tightly correlated with the inferred gas depletion time, whether based on the stellar surface mass density or the orbital dynamical time. This suggests that we are seeing the response of a simple gas-regulator system to variations in the accretion rate. This is explored using a heuristic model that can quantitatively explain the dependence of σ(ΣSFR) on gas depletion timescale. Variations in accretion rate are progressively more damped out in regions of low star-formation efficiency leading to a reduced amplitude of variations in star-formation. AU - Wang, Enci AU - Lilly, Simon J. AU - Pezzulli, Gabriele AU - Matthee, Jorryt J ID - 11517 IS - 2 JF - The Astrophysical Journal KW - Space and Planetary Science KW - Astronomy and Astrophysics SN - 0004-637X TI - On the elevation and suppression of star formation within galaxies VL - 877 ER - TY - JOUR AB - We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12 M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent correlation between halo mass and Ly α luminosity normalized by the characteristic Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs (L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame 1500 Å UV luminosity, MUV, is also observed where the halo masses increase from 1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to 10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority of those sources are active galactic nuclei. All the trends we observe are found to be redshift independent. Our results reveal that LAEs are the likely progenitors of a wide range of galaxies depending on their luminosity, from dwarf-like, to Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight into the early formation and evolution of the galaxies we observe in the local Universe. AU - Khostovan, A A AU - Sobral, D AU - Mobasher, B AU - Matthee, Jorryt J AU - Cochrane, R K AU - Chartab, N AU - Jafariyazani, M AU - Paulino-Afonso, A AU - Santos, S AU - Calhau, J ID - 11535 IS - 1 JF - Monthly Notices of the Royal Astronomical Society KW - Space and Planetary Science KW - Astronomy and Astrophysics KW - galaxies: evolution KW - galaxies: haloes KW - galaxies: high-redshift KW - galaxies: star formation KW - cosmology: observations KW - large-scale structure of Universe SN - 0035-8711 TI - The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities VL - 489 ER - TY - JOUR AB - We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV) lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7 (COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7 reveal an He II emission line in observations obtained along the major axis of Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8 arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3 grism spectra detects the UV continuum of CR7’s clump A, yielding a power law with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20⁠. No significant variability is found for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2 (3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing nature of CR7. CR7 seems to be actively forming stars without any clear active galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙. Component C or an interclump component between B and C may host a high ionization source. Our results highlight the need for spatially resolved information to study the formation and assembly of early galaxies. AU - Sobral, David AU - Matthee, Jorryt J AU - Brammer, Gabriel AU - Ferrara, Andrea AU - Alegre, Lara AU - Röttgering, Huub AU - Schaerer, Daniel AU - Mobasher, Bahram AU - Darvish, Behnam ID - 11541 IS - 2 JF - Monthly Notices of the Royal Astronomical Society KW - Space and Planetary Science KW - Astronomy and Astrophysics KW - galaxies: evolution KW - galaxies: high-redshift KW - galaxies: ISM KW - cosmology: observations KW - dark ages KW - reionization KW - first stars KW - early Universe SN - 0035-8711 TI - On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components VL - 482 ER - TY - JOUR AB - Observations have revealed that the star formation rate (SFR) and stellar mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy main sequence. However, what physical information is encoded in this relation is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar relation. At z = 0, we find that the scatter decreases slightly with stellar mass from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for lower masses. We show that the scatter at z = 0.1 originates from a combination of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably associated with self-regulation from cooling, star formation, and outflows, but is dominated by long time-scale (∼10 Gyr) variations related to differences in halo formation times. Shorter time-scale fluctuations are relatively more important for lower mass galaxies. At high masses, differences in black hole formation efficiency cause additional scatter, but also diminish the scatter caused by different halo formation times. While individual galaxies cross the main sequence multiple times during their evolution, they fluctuate around tracks associated with their halo properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have been above/below the main sequence for ≫1 Gyr. AU - Matthee, Jorryt J AU - Schaye, Joop ID - 11540 IS - 1 JF - Monthly Notices of the Royal Astronomical Society KW - Space and Planetary Science KW - Astronomy and Astrophysics : galaxies: evolution KW - galaxies: formation KW - galaxies: star formation KW - cosmology: theory SN - 0035-8711 TI - The origin of scatter in the star formation rate–stellar mass relation VL - 484 ER - TY - JOUR AB - We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V = 8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (R⋆ = 2.943 ± 0.064 R⊙), mass (M⋆ = 1.212 ± 0.074 M⊙), and age (4.9 ± 1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a "hot Saturn" (Rp = 9.17 ± 0.33 R⊕) with an orbital period of ∼14.3 days, irradiance of F = 343 ± 24 F⊕, and moderate mass (Mp = 60.5 ± 5.7 M⊕) and density (ρp = 0.431 ± 0.062 g cm−3). The properties of HD 221416 b show that the host-star metallicity–planet mass correlation found in sub-Saturns (4–8 R⊕) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology. AU - Huber, Daniel AU - Chaplin, William J. AU - Chontos, Ashley AU - Kjeldsen, Hans AU - Christensen-Dalsgaard, Jørgen AU - Bedding, Timothy R. AU - Ball, Warrick AU - Brahm, Rafael AU - Espinoza, Nestor AU - Henning, Thomas AU - Jordán, Andrés AU - Sarkis, Paula AU - Knudstrup, Emil AU - Albrecht, Simon AU - Grundahl, Frank AU - Andersen, Mads Fredslund AU - Pallé, Pere L. AU - Crossfield, Ian AU - Fulton, Benjamin AU - Howard, Andrew W. AU - Isaacson, Howard T. AU - Weiss, Lauren M. AU - Handberg, Rasmus AU - Lund, Mikkel N. AU - Serenelli, Aldo M. AU - Rørsted Mosumgaard, Jakob AU - Stokholm, Amalie AU - Bieryla, Allyson AU - Buchhave, Lars A. AU - Latham, David W. AU - Quinn, Samuel N. AU - Gaidos, Eric AU - Hirano, Teruyuki AU - Ricker, George R. AU - Vanderspek, Roland K. AU - Seager, Sara AU - Jenkins, Jon M. AU - Winn, Joshua N. AU - Antia, H. M. AU - Appourchaux, Thierry AU - Basu, Sarbani AU - Bell, Keaton J. AU - Benomar, Othman AU - Bonanno, Alfio AU - Buzasi, Derek L. AU - Campante, Tiago L. AU - Çelik Orhan, Z. AU - Corsaro, Enrico AU - Cunha, Margarida S. AU - Davies, Guy R. AU - Deheuvels, Sebastien AU - Grunblatt, Samuel K. AU - Hasanzadeh, Amir AU - Di Mauro, Maria Pia AU - A. García, Rafael AU - Gaulme, Patrick AU - Girardi, Léo AU - Guzik, Joyce A. AU - Hon, Marc AU - Jiang, Chen AU - Kallinger, Thomas AU - Kawaler, Steven D. AU - Kuszlewicz, James S. AU - Lebreton, Yveline AU - Li, Tanda AU - Lucas, Miles AU - Lundkvist, Mia S. AU - Mann, Andrew W. AU - Mathis, Stéphane AU - Mathur, Savita AU - Mazumdar, Anwesh AU - Metcalfe, Travis S. AU - Miglio, Andrea AU - F. G. Monteiro, Mário J. P. AU - Mosser, Benoit AU - Noll, Anthony AU - Nsamba, Benard AU - Joel Ong, Jia Mian AU - Örtel, S. AU - Pereira, Filipe AU - Ranadive, Pritesh AU - Régulo, Clara AU - Rodrigues, Thaíse S. AU - Roxburgh, Ian W. AU - Aguirre, Victor Silva AU - Smalley, Barry AU - Schofield, Mathew AU - Sousa, Sérgio G. AU - Stassun, Keivan G. AU - Stello, Dennis AU - Tayar, Jamie AU - White, Timothy R. AU - Verma, Kuldeep AU - Vrard, Mathieu AU - Yıldız, M. AU - Baker, David AU - Bazot, Michaël AU - Beichmann, Charles AU - Bergmann, Christoph AU - Bugnet, Lisa Annabelle AU - Cale, Bryson AU - Carlino, Roberto AU - Cartwright, Scott M. AU - Christiansen, Jessie L. AU - Ciardi, David R. AU - Creevey, Orlagh AU - Dittmann, Jason A. AU - Nascimento, Jose-Dias Do AU - Eylen, Vincent Van AU - Fürész, Gabor AU - Gagné, Jonathan AU - Gao, Peter AU - Gazeas, Kosmas AU - Giddens, Frank AU - Hall, Oliver J. AU - Hekker, Saskia AU - Ireland, Michael J. AU - Latouf, Natasha AU - LeBrun, Danny AU - Levine, Alan M. AU - Matzko, William AU - Natinsky, Eva AU - Page, Emma AU - Plavchan, Peter AU - Mansouri-Samani, Masoud AU - McCauliff, Sean AU - Mullally, Susan E. AU - Orenstein, Brendan AU - Soto, Aylin Garcia AU - Paegert, Martin AU - van Saders, Jennifer L. AU - Schnaible, Chloe AU - Soderblom, David R. AU - Szabó, Róbert AU - Tanner, Angelle AU - Tinney, C. G. AU - Teske, Johanna AU - Thomas, Alexandra AU - Trampedach, Regner AU - Wright, Duncan AU - Yuan, Thomas T. AU - Zohrabi, Farzaneh ID - 11616 IS - 6 JF - The Astronomical Journal KW - Space and Planetary Science KW - Astronomy and Astrophysics SN - 0004-6256 TI - A hot Saturn orbiting an oscillating late subgiant discovered by TESS VL - 157 ER - TY - JOUR AB - Over 2,000 stars were observed for 1 month with a high enough cadence in order to look for acoustic modes during the survey phase of the Kepler mission. Solar-like oscillations have been detected in about 540 stars. The question of why no oscillations were detected in the remaining stars is still open. Previous works explained the non-detection of modes with the high level of magnetic activity of the stars. However, the sample of stars studied contained some classical pulsators and red giants that could have biased the results. In this work, we revisit this analysis on a cleaner sample of main-sequence solar-like stars that consists of 1,014 stars. First we compute the predicted amplitude of the modes of that sample and for the stars with detected oscillation and compare it to the noise at high frequency in the power spectrum. We find that the stars with detected modes have an amplitude to noise ratio larger than 0.94. We measure reliable rotation periods and the associated photometric magnetic index for 684 stars out of the full sample and in particular for 323 stars where the amplitude of the modes is predicted to be high enough to be detected. We find that among these 323 stars 32% of them have a level of magnetic activity larger than the Sun during its maximum activity, explaining the non-detection of acoustic modes. Interestingly, magnetic activity cannot be the primary reason responsible for the absence of detectable modes in the remaining 68% of the stars without acoustic modes detected and with reliable rotation periods. Thus, we investigate metallicity, inclination angle of the rotation axis, and binarity as possible causes of low mode amplitudes. Using spectroscopic observations for a subsample, we find that a low metallicity could be the reason for suppressed modes. No clear correlation with binarity nor inclination is found. We also derive the lower limit for our photometric activity index (of 20–30 ppm) below which rotation and magnetic activity are not detected. Finally, with our analysis we conclude that stars with a photometric activity index larger than 2,000 ppm have 98.3% probability of not having oscillations detected. AU - Mathur, Savita AU - García, Rafael A. AU - Bugnet, Lisa Annabelle AU - Santos, Ângela R.G. AU - Santiago, Netsha AU - Beck, Paul G. ID - 11613 JF - Frontiers in Astronomy and Space Sciences KW - Astronomy and Astrophysics TI - Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler VL - 6 ER -