KELT-1b: A STRONGLY IRRADIATED, HIGHLY INFLATED, SHORT PERIOD, 27 JUPITER-MASS COMPANION TRANSITING A MID-F STAR

Siverd, Robert J.; Beatty, Thomas G.; Pepper, Joshua; Eastman, Jason D.; Collins, Karen A.; Bieryla, Allyson; Latham, David W.; Buchhave, Lars A.; Jensen, Eric L. N.; Crepp, Justin R.; Street, R. A.; Stassun, Keivan G.; Gaudi, B. Scott; Berlind, P.; Calkins, M.; DePoy, D. L.; Esquerdo, Gilbert A.; Fulton, Benjamin J.; Fürész, Gábor; Geary, John C.; Gould, Andrew; Hebb, Leslie; Kielkopf, John F.; Marshall, J. L.; Pogge, Richard W.; Stanek, K. Z.; Stefanik, R. P.; Szentgyorgyi, Andrew; Trueblood, Mark; Trueblood, Patricia; Stutz, Amelia M.; Saders, Jennifer L. van

doi:10.1088/0004-637x/761/2/123

Cited by 258 publications

(221 citation statements)

References 188 publications

(213 reference statements)

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“…We approximate the all observations to the AAVSO V-band to match the quiescent magnitude of the AAVSO data but no attempt has been made to place all the data on the same absolute scale. ISIS software package, described further in Section 2 of Siverd et al (2012). The photometric scatter (outside the eclipse) of the KELT-North light curve for TYC 2505-672-1 is ∼2%, roughly consistent with the expected scatter for a target of this brightness located at its position in the KELT-North field.…”

Section: Kelt-northsupporting

confidence: 60%

An EXTREME ANALOGUE OF Ε AURIGAE: AN M-Giant ECLIPSED EVERY 69 YEARS BY a LARGE OPAQUE DISK SURROUNDING a SMALL HOT SOURCE

Rodriguez

Stassun

Lund

et al. 2016

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We present TYC 2505-672-1 as a newly discovered and remarkable eclipsing system comprising an M-type red giant that undergoes a ∼3.45 year long, near-total eclipse (depth of ∼4.5 mag) with a very long period of ∼69.1 years. TYC 2505-672-1 is now the longest-period eclipsing binary system yet discovered, more than twice as long as that of the currently longest-period system, ò Aurigae. We show from analysis of the light curve including both our own data and historical data spanning more than 120 years and from modeling of the spectral energy distribution, both before and during eclipse, that the red giant primary is orbited by a moderately hot source (T eff ≈ 8000 K) that is itself surrounded by an extended, opaque circumstellar disk. From the measured ratio of luminosities, the radius of the hot companion must be in the range of 0.1-0.5 R e (depending on the assumed radius of the red giant primary), which is an order of magnitude smaller than that for a main sequence A star and 1-2 orders of magnitude larger than that for a white dwarf. The companion is therefore most likely a "stripped red giant" subdwarf-B type star destined to become a He white dwarf. It is, however, somewhat cooler than most sdB stars, implying a very low mass for this "pre-He-WD" star. The opaque disk surrounding this hot source may be a remnant of the stripping of its former hydrogen envelope. However, it is puzzling how this object became stripped, given that it is at present so distant (orbital semimajor axis of ∼24 au) from the current red giant primary star. Extrapolating from our calculated ephemeris, the next eclipse should begin in early UT 2080 April and end in mid UT 2083 September (eclipse center UT 2081 December 24). In the meantime, radial velocity observations would establish the masses of the components, and highcadence UV observations could potentially reveal oscillations of the hot companion that would further constrain its evolutionary status. In any case, this system is poised to become an exemplar of a very rare class of systems, even more extreme in several respects than the well studied archetype ò Aurigae.

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Section: Kelt-northsupporting

confidence: 60%

An EXTREME ANALOGUE OF Ε AURIGAE: AN M-Giant ECLIPSED EVERY 69 YEARS BY a LARGE OPAQUE DISK SURROUNDING a SMALL HOT SOURCE

Rodriguez

Stassun

Lund

et al. 2016

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“…Images from a single observatory and a single filter were registered to a common alignment using the Sexterp routine (Siverd et al 2012). We then employed the ISIS image subtraction package (Alard & Lupton 1998;Alard 2000) to build a reference image (Figure 1) from the subset of images taken under the best conditions.…”

Section: Photometrymentioning

confidence: 99%

A Reverberation-Based Black Hole Mass for McG-06-30-15

Bentz

Cackett

Crenshaw

et al. 2016

ApJ

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We present the results of a reverberation campaign targeting MGC-06-30-15. Spectrophotometric monitoring and broad-band photometric monitoring over the course of four months in spring 2012 allowed a determination of a time delay in the broad Hβ emission line of τ=5.3±1.8 days in the rest frame of the active galactic nucleus (AGN). Combined with the width of the variable portion of the emission line, we determine a black hole mass of M BH =(1.6 ± 0.4)×106 M e . Both the Hβ time delay and the black hole mass are in good agreement with expectations from the R BLR -L and M BH -σ å relationships for other reverberation-mapped AGNs. The Hβ time delay is also in good agreement with the relationship between Hβ and broad-band near-IR delays, in which the effective size of the broad-line region is ∼4-5 times smaller than the inner edge of the dust torus. Additionally, the reverberation-based mass is in good agreement with estimates from the scaling relationship of the break in the X-ray power spectral density, and with constraints based on stellar kinematics derived from integral field spectroscopy of the inner ∼0.5 kpc of the galaxy.

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“…The KELT-North telescope observed V1334 Tau from UT 2006 October 26 to UT 2013 March 13, obtaining 9186 observations after processing. For a detailed description of the KELT data acquisition and reduction process, see Siverd et al (2012). The median per-point error is 0.005 mag.…”

Section: Keltmentioning

confidence: 99%

The Mysterious Dimmings of the T Tauri Star V1334 Tau

Rodriguez

Zhou

Cargile

et al. 2017

ApJ

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We present the discovery of two extended ∼0.12 mag dimming events of the weak-lined T Tauri star V1334. The start of the first event was missed but came to an end in late 2003, and the second began in 2009 February, and continues as of 2016 November. Since the egress of the current event has not yet been observed, it suggests a period of >13 years if this event is periodic. Spectroscopic observations suggest the presence of a small inner disk, although the spectral energy distribution shows no infrared excess. We explore the possibility that the dimming events are caused by an orbiting body (e.g., a disk warp or dust trap), enhanced disk winds, hydrodynamical fluctuations of the inner disk, or a significant increase in the magnetic field flux at the surface of the star. We also find a ∼0.32 day periodic photometric signal that persists throughout the 2009 dimming which appears to not be due to ellipsoidal variations from a close stellar companion. High-precision photometric observations of V1334 Tau during K2 campaign 13, combined with simultaneous photometric and spectroscopic observations from the ground, will provide crucial information about the photometric variability and its origin.

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KELT-1b: A STRONGLY IRRADIATED, HIGHLY INFLATED, SHORT PERIOD, 27 JUPITER-MASS COMPANION TRANSITING A MID-F STAR

Cited by 258 publications

References 188 publications

An EXTREME ANALOGUE OF Ε AURIGAE: AN M-Giant ECLIPSED EVERY 69 YEARS BY a LARGE OPAQUE DISK SURROUNDING a SMALL HOT SOURCE

An EXTREME ANALOGUE OF Ε AURIGAE: AN M-Giant ECLIPSED EVERY 69 YEARS BY a LARGE OPAQUE DISK SURROUNDING a SMALL HOT SOURCE

A Reverberation-Based Black Hole Mass for McG-06-30-15

The Mysterious Dimmings of the T Tauri Star V1334 Tau

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