INITIAL PERFORMANCE OF THE<i>NEOWISE</i>REACTIVATION MISSION

Mainzer, Amy; Bauer, J. M.; Cutri, R. M.; Grav, T.; Masiero, J.; Beck, R.; Clarkson, P.; Conrow, T.; Dailey, J.; Eisenhardt, Peter; Fabinsky, Beth; Fajardo-Acosta, S. B.; Fowler, J. W.; Gelino, Christopher R.; Grillmair, Carl J.; Heinrichsen, I.; Kendall, M.; Kirkpatrick, J. Davy; Liu, F.; Masci, Frank J.; McCallon, H.; Nugent, C.; Papin, M.; Rice, Emily L.; Royer, D.; Ryan, Thomas Curran; Sevilla, P.; Sonnett, S.; Stevenson, R.; Thompson, D. B.; Wheelock, S.; Wiemer, Doug; Wittman, M.; Wright, E. L.; Yan, Lin

doi:10.1088/0004-637x/792/1/30

Cited by 573 publications

(382 citation statements)

References 46 publications

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“…They predicted that the dust emission, whichpeaked at 3-10 μm, has a typical luminosity between 10 42-43 erg s −1 in the case of well studied TDE ASASSN-14li (e.g., Miller et al 2015;Alexander et al 2016;Holoien et al 2016;van Velzen et al 2016a), if most UV light is reprocessed into infrared. We confirmed such a mid-IR echo in ASASSN-14li, which lags the detected optical flare by ∼36 days (Jiang et al 2016), based on the WISE cryogenic and NEOWISE post-cryogenic survey (hereafter ALLWISE Release) and NEOWISE Reactivation Survey (hereafter NEOWISE-R) at 3.4 and 4.6 μm (labeled as W1 and W2, Wright et al 2010;Mainzer et al 2011Mainzer et al , 2014;though, the luminosity in the infrared band is one to twoordersof magnitude lower than the model prediction due to low dust content.…”

Section: Introductionsupporting

confidence: 65%

Long Fading Mid-Infrared Emission in Transient Coronal Line Emitters: Dust Echo of a Tidal Disruption Flare

Dou¹,

Wang²,

Jiang³

et al. 2016

ApJ

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The sporadic accretion following the tidal disruption of a star by a super-massive black hole (TDE) leads to a brightUV and soft X-ray flare in the galactic nucleus. The gas and dust surrounding the black hole responses to such a flare with an echo in emission lines and infrared emission. In this paper, we report the detection of long fading mid-IR emission lasting up to 14 years after the flare in four TDE candidates with transient coronal lines using the WISE public data release. We estimate that the reprocessed mid-IR luminosities are in the range betweeń 4 10 42 and2 10 43 erg s −1 and dust temperature in the range of 570-800 K when WISE first detected these sources three to five years after the flare. Both luminosity and dust temperature decrease with time. We interpret the mid-IR emission as the infrared echo of the tidal disruption flare. We estimate the UV luminosity at the peak flare to be 1to 30 times 10 44 erg s −1 and that forwarm dust masses to bein the range of 0.05-1.3  M within a few parsecs. Our results suggest that themid-infrared echo is a general signature of TDE in the gas-rich environment.

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Section: Introductionsupporting

confidence: 65%

Long Fading Mid-Infrared Emission in Transient Coronal Line Emitters: Dust Echo of a Tidal Disruption Flare

Dou¹,

Wang²,

Jiang³

et al. 2016

ApJ

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“…To measure the properties of the Milky Way's X/P structure, we use two wide-field, infrared images (at 3.4 and 4.6 µm) of the Galaxy, observed with the Wide-field Infrared Survey Explorer (wise) satellite (Wright et al 2010, Mainzer et al 2014. The images are identical to those used in Ness & Lang (2016) except that they cover a slightly wider field of view.…”

Section: Wise Datamentioning

confidence: 99%

Quantifying the (X/peanut)-shaped structure of the Milky Way – new constraints on the bar geometry

Ciambur

Graham

Bland-Hawthorn

2017

Monthly Notices of the Royal Astronomical Society

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The nature, size and orientation of the dominant structural components in the Milky Way's inner ∼ 4 kpc -specifically the bulge and bar -have been the subject of conflicting interpretations in the literature. We present a different approach to inferring the properties of the long bar which extends beyond the inner bulge, via the information encoded in the Galaxy's X/peanut (X/P)-shaped structure. We perform a quantitative analysis of the X/P feature seen in wise wide-field imaging at 3.4 µm and 4.6 µm. We measure the deviations of the isophotes from pure ellipses, and quantify the X/P structure via the radial profile of the Fourier n = 6 harmonic (cosine term B 6 ). In addition to the vertical height and integrated 'strength' of the X/P instability, we report an intrinsic radius of R Π ,int = 1.67 ± 0.27 kpc, and an orientation angle of α = 37•+7• −10 • with respect to our line-of-sight to the Galactic Centre. Based on X/P structures observed in other galaxies, we make three assumptions: (i) the peanut is intrinsically symmetric, (ii) the peanut is aligned with the long Galactic bar, and (iii) their sizes are correlated. Thus the implication for the Galactic bar is that it is oriented at the same 37• angle and has an expected radius of ≈ 4.2 kpc, but possibly as low as ≈ 3.2 kpc. We further investigate how the Milky Way's X/P structure compares with other analogues, and find that the Galaxy is broadly consistent with our recently established scaling relations, though with a moderately stronger peanut instability than expected. We additionally perform a photometric decomposition of the Milky Way's major axis surface brightness profile, accounting for spiral structure, and determine an average disc scale length of h = 2.54 ± 0.16 kpc in the wise bands, in good agreement with the literature.

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“…The SAGE-VAR program followed up with four more epochs in the core of the SMC from 2010 to 2011 ("VAR" refers to the focus of this program on variable stars; Riebel et al 2015). The WISE data include the reactivated mission to study near-Earth Objects (NEOWISE-R; Mainzer et al 2014). The all-sky scanning strategy for WISE covers the SMC every six months, giving two epochs in 2010 and four in the period 2014-2015.…”

Section: A2 Mean Photometrymentioning

confidence: 99%

Characterizing the Population of Bright Infrared Sources in the Small Magellanic Cloud

Kraemer

Sloan

Wood

et al. 2017

ApJ

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We used Spitzer's Infrared Spectrograph (IRS) to observe stars in the Small Magellanic Cloud (SMC) selected from the Midcourse Space Experiment (MSX) Point Source Catalog. We concentrate on the dust properties of oxygen-rich evolved stars, which show less alumina than Galactic stars. This difference may arise from the SMC's lower metallicity, but it could be a selection effect: the SMC sample includes more stars which are brighter and thus more massive. The distribution of SMC stars along the silicate sequence looks more like that of Galactic red supergiants than asymptotic giant branch stars (AGBs). While many are definitively AGBs, several SMC stars show evidence of hot bottom burning. Other sources show mixed chemistry (oxygen-rich and carbon-rich features), including supergiants with PAH emission. MSX SMC 134 may be the first confirmed silicate/carbon star in the SMC, and MSX SMC 049 is a post-AGB candidate. MSX SMC 145, previously a candidate OH/IR star, is actually an AGB star with a background galaxy at z=0.16 along the same line-of-sight. We consider the overall characteristics of all the MSX sources, the most infrared-bright objects in the SMC, in light of Spitzer's higher sensitivity and resolution, and compare them with the object types expected from the original selection criteria. This population represents what will be seen in more distant galaxies by the James Webb Space Telescope (JWST). Color-color diagrams using the IRS spectra and JWST mid-infrared filters show how one can separate evolved stars from young stellar objects (YSOs) and distinguish among different YSO classes.

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INITIAL PERFORMANCE OF THENEOWISEREACTIVATION MISSION

Cited by 573 publications

References 46 publications

Long Fading Mid-Infrared Emission in Transient Coronal Line Emitters: Dust Echo of a Tidal Disruption Flare

Long Fading Mid-Infrared Emission in Transient Coronal Line Emitters: Dust Echo of a Tidal Disruption Flare

Quantifying the (X/peanut)-shaped structure of the Milky Way – new constraints on the bar geometry

Characterizing the Population of Bright Infrared Sources in the Small Magellanic Cloud

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