MMT and Magellan Infrared Spectrograph

McLeod, B. A.; Fabricant, Daniel G.; Nystrom, G.; McCracken, K. G.; Amato, Stephen M.; Bergner, Henry; Brown, Warren R.; Burke, Michael W.; Chilingarian, Igor; Conroy, Maureen A.; Curley, Dylan; Fürész, Gábor; Geary, John C.; Hertz, Edward; Holwell, Justin; Matthews, Anne; Park, Sang C.; Roll, John; Zajac, Joseph; Epps, Harland W.; Martini, Paul

doi:10.1086/669044

Cited by 63 publications

(43 citation statements)

References 30 publications

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“…We obtained two spectra of J0047 separated by about one year: one with the MMT and Magellan Infrared Spectrograph (MMIRS;McLeod et al 2012) on the Magellan Clay telescope at Las Campanas Observatory, and the other with X-shooter (Vernet et al 2011) on the Very Large Telescope (VLT) UT3 at Cerro Paranal.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Discovery of a red supergiant counterpart to RX J004722.4–252051, a ULX in NGC 253

Heida

Torres

Jonker

et al. 2015

Mon. Not. R. Astron. Soc.

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We present two epochs of near-infrared spectroscopy of the candidate red supergiant counterpart to RX J004722.4-252051, a ULX in NGC 253. We measure radial velocities of the object and its approximate spectral type by cross-correlating our spectra with those of known red supergiants. Our VLT/X-shooter spectrum is best matched by that of early M-type supergiants, confirming the red supergiant nature of the candidate counterpart. The radial velocity of the spectrum, taken on 2014, August 23, is 417 ± 4 km s −1 . This is consistent with the radial velocity measured in our spectrum taken with Magellan/MMIRS on 2013, June 28, of 410 ± 70 km s −1 , although the large error on the latter implies that a radial velocity shift expected for a black hole of tens of M can easily be hidden. Using nebular emission lines we find that the radial velocity due to the rotation of NGC 253 is 351 ± 4 km s −1 at the position of the ULX. Thus the radial velocity of the counterpart confirms that the source is located in NGC 253, but also shows an offset with respect to the local bulk motion of the galaxy of 66 ± 6 km s −1 . We argue that the most likely origin for this displacement lies either in a SN kick, requiring a system containing a 50 M black hole, and/or in orbital radial velocity variations in the ULX binary system, requiring a 100 M black hole. We therefore conclude that RX J004722.4-252051 is a strong candidate for a ULX containing a massive stellar black hole.

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Section: Observations and Data Reductionmentioning

confidence: 99%

Discovery of a red supergiant counterpart to RX J004722.4–252051, a ULX in NGC 253

Heida

Torres

Jonker

et al. 2015

Mon. Not. R. Astron. Soc.

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“…It is detectable because of photoionization and heating by the X-ray and EUV emission from gas heated by the forward and reverse shocks. This paper reports deep IR spectra of diffuse emission inside Cas A obtained with the MMT/Magellan Infrared Spectrograph (MMIRS) instrument on the 6.5 m MMT telescope (McLeod et al 2012). The diffuse emission appears in a deep 1.64 µm image from UKIRT (Koo et al 2018) as a smooth, faint emission region interior to the shell of FMKs.…”

Section: Introductionmentioning

confidence: 99%

The Temperature and Ionization of Unshocked Ejecta in Cas A

Raymond

Koo

Lee

et al. 2018

ApJ

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The supernova remnant Cassiopeia A (Cas A) is one of the few remnants in which it is possible to observe unshocked ejecta. A deep 1.64 µm image of Cas A shows a patch of diffuse emission from unshocked ejecta, as well as brighter emission from Fast-Moving Knots and Quasi-Stationary Flocculi. Emission at 1.64 µm is usually interpreted as [Fe II] emission, and spectra of the bright knots confirm this by showing the expected emission in other [Fe II] lines. We performed NIR spectroscopy on the diffuse emission region and found that the unshocked ejecta emission does not show those lines, but rather the [Si I] 1.607 µm line. This means that the 1.64 µm line from the unshocked ejecta may be the [Si I] 1.645 line from the same upper level, rather than [Fe II]. We find that the [Si I] line is formed by recombination, and we use the [Si I] to [Si II] ratio to infer a temperature about 100 K, close to the value assumed for analysis of low frequency radio absorption and that inferred from emission by cool dust. Our results constrain estimates of Cas A's total mass of unshocked ejecta that are extremely sensitive to temperature assumptions, but they do not resolve the ambiguity due to clumping.

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“…A complete sample of such proplyds has been cataloged in Ricci et al (2008). For our investigation, with the MMT and Magellan infrared spectrograph (MMIRS; McLeod et al 2012) mounted on the MMT telescope, we performed near-infrared spectroscopic observations of the central stars in a subsample of the proplyds (M. Fang et al 2016, in preparation).…”

Section: Introductionmentioning

confidence: 99%

A Candidate Planetary-Mass Object With a Photoevaporating Disk in Orion

Fang

Kim

Pascucci

et al. 2016

ApJL

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In this work, we report the discovery of a candidate planetary-mass object with a photoevaporating protoplanetary disk, Proplyd133-353, which is near the massive star θ 1 Ori C at the center of the Orion Nebula Cluster (ONC). The object was known to have extended emission pointing away from θ 1 OriC, indicating ongoing external photoevaporation. Our near-infrared spectroscopic data and the location on the H-R diagram suggest that the central source of Proplyd133-353 is substellar (∼M9.5) and has a mass probably less than 13 Jupiter mass and an age younger than 0.5 Myr. Proplyd133-353 shows a similar ratio of X-ray luminosity to stellar luminosity to other young stars in the ONC with a similar stellar luminosity and has a similar proper motion to the mean one of confirmed ONC members. We propose that Proplyd133-353 formed in a very low-mass dusty cloud or an evaporating gas globule near θ 1 Ori C as a second generation of star formation, which can explain both its young age and the presence of its disk.

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MMT and Magellan Infrared Spectrograph

Cited by 63 publications

References 30 publications

Discovery of a red supergiant counterpart to RX J004722.4–252051, a ULX in NGC 253

Discovery of a red supergiant counterpart to RX J004722.4–252051, a ULX in NGC 253

The Temperature and Ionization of Unshocked Ejecta in Cas A

A Candidate Planetary-Mass Object With a Photoevaporating Disk in Orion

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