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 -