Spextool: A Spectral Extraction Package for SpeX, a 0.8–5.5 Micron Cross‐Dispersed Spectrograph

Cushing, Michael C.; Vacca, William D.; Rayner, John

doi:10.1086/382907

Cited by 1,062 publications

(480 citation statements)

References 14 publications

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“…The A0-type standard stars HD 79752 and HD 91398 were observed immediately after the science targets and at a similar airmass to correct for telluric absorption and instrument response. The data were reduced using the IDL SpeXTool v4.0 beta package 4 (Vacca et al 2003;Cushing et al 2004). …”

Section: Spex At Irtfmentioning

confidence: 99%

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

Gagné

Faherty

Mamajek

et al. 2017

ApJS

102

106

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A determination of the initial mass function (IMF) of the current, incomplete census of the 10 Myrold TW Hya association (TWA) is presented. This census is built from a literature compilation supplemented with new spectra and 17 new radial velocities from on-going membership surveys, as well as a re-analysis of Hipparcos data that confirmed HR 4334 (A2 Vn) as a member. Though the dominant uncertainty in the IMF remains census incompleteness, a detailed statistical treatment is carried out to make the IMF determination independent of binning, while accounting for small number statistics. The currently known high-likelihood members are fitted by a log-normal distribution with a central mass of 0.21−0.06 M and a characteristic width of 0.8 +0.2 −0.1 dex in the 12 M Jup -2 M range, whereas a Salpeter power law with α = 2.2 +1.1 −0.5 best describes the IMF slope in the 0.1-2 M range. This characteristic width is higher than other young associations, which may be due to incompleteness in the current census of low-mass TWA stars. A tentative overpopulation of isolated planetary-mass members similar to 2MASS J11472421-2040204 and 2MASS J11193254-1137466 is identified: this indicates that there might be as many as 10 +13 −5 similar members of TWA with hot-start modeldependent masses estimated at ∼ 5-7 M Jup , most of which would be too faint to be detected in 2MASS . Our new radial velocity measurements corroborate the membership of 2MASS J11472421-2040204, and secure TWA 28 (M8.5 γ), TWA 29 (M9.5 γ) and TWA 33 (M4.5 e) as members. The discovery of 2MASS J09553336-0208403, a young L7-type interloper unrelated to TWA, is also presented.

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Section: Spex At Irtfmentioning

confidence: 99%

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

Gagné

Faherty

Mamajek

et al. 2017

ApJS

102

106

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“…Next, we used standard IRAF procedures to produce a 1D spectrum, using an aperture of 11 pix (i.e., 2 ′′ ). Finally, we used the Spextool IDL package to remove the telluric absorption features near 2 µm and to perform the relative and absolute flux calibrations, based on a detailed library spectrum of Vega (32,33). The absolute flux calibration we obtained is in excellent agreement with the archival photometry available for CID-947: the synthetic magnitude derived from the spectrum is K s = 20.03 (AB magnitudes), compared with the archival value of 20.00 ± 0.01 (34).…”

Section: S11 Keck/mosfire Observations and Data Reductionmentioning

confidence: 99%

An over-massive black hole in a typical star-forming galaxy, 2 billion years after the Big Bang

Trakhtenbrot

Urry

Civano

et al. 2015

Science

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Supermassive black holes (SMBHs) and their host galaxies are generally thought to coevolve, so that the SMBH achieves up to about 0.2 to 0.5% of the host galaxy mass in the present day. The radiation emitted from the growing SMBH is expected to affect star formation throughout the host galaxy. The relevance of this scenario at early cosmic epochs is not yet established. We present spectroscopic observations of a galaxy at redshift z = 3.328, which hosts an actively 1 accreting, extremely massive BH, in its final stages of growth. The SMBH mass is roughly one-tenth the mass of the entire host galaxy, suggesting that it has grown much more efficiently than the host, contrary to models of synchronized coevolution. The host galaxy is forming stars at an intense rate, despite the presence of a SMBH-driven gas outflow.Several lines of observational evidence, spanning a wide range of cosmic epochs, have led to a commonly accepted picture wherein supermassive black holes (SMBHs, M BH > 10 6 M ⊙ ; M ⊙ is the solar mass) coevolve with their host galaxies (1-4). Moreover, energy-and/or momentumdriven "feedback" from accreting SMBHs (Active Galactic Nuclei; AGN) is thought to quench star formation in the host galaxy (5). To directly test the relevance of such scenarios at early cosmic epochs (high redshifts, z) requires the most basic properties of SMBHs and their hosts, including masses and growth rates, to be observed. Several observational studies found that at z < ∼ 2 (more than 3.3 billion years after the Big Bang), the typical BH-to-stellar mass ratio, CID-947 is an x-ray-selected, unobscured AGN at z = 3.328, detected in both XMM-Newtonand Chandra x-ray imaging data of the COSMOS field [see Fig. S4 and sections S2 and S4 in the supplementary materials (16)]. We obtained a near-infrared (IR) K-band spectrum of CID-947 using the MOSFIRE instrument at the W. M. Keck telescope, which at z = 3.328 covers the hydrogen Hβ broad emission line (see details in section S1 in the supplementary materials).The calibrated spectrum shows a very broad Hβ emission line, among other features ( Fig. 1).Our spectral analysis indicates that the monochromatic AGN luminosity at rest-frame 5100Åis L 5100 = 3.58 By combining this line width with the observed L 5100 and relying on an empirically calibrated estimator for M BH , based on the virial motion of ionized gas near the SMBH (17), we obtain M BH = 6.9All the reported measurement-related uncertainties are derived by a series of simulations and represent the 16th and 84th quantiles of the resulting distributions.These simulations indicate a SMBH mass larger than 3.6 × 10 9 M ⊙ at the 99% confidence level (see sections S1.2 and S3 for more details). Determinations of M BH from single-epoch spectra of the Hβ emission line are known to also be affected by significant systematic uncertainties, of up to ∼ 0.3 to 0.4 dex. For a detailed discussion of some of the systematics and related issues, see §S3 in the supplementary materials. This high M BH is comparable with some of the most massive BHs...

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“…The main difference is that in addition to the solar analogs, and in order to correct for telluric water vapor features, local standard stars are also observed. Due to a higher and more variable background at NIR wavelengths exposures were limited to 120 s. SpeX data were reduced with Spextool (Cushing et al, 2004). NIR spectra are normalized to unity at 1.4 µm.…”

Section: Near-infrared Spectramentioning

confidence: 99%

Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids

Sanchez

Michelsen

Reddy

et al. 2013

Icarus

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In the past, constraining the surface composition of near-Earth asteroids (NEAs) has been difficult due to the lack of high quality near-IR spectral data (0.7-2.5 µm) that contain mineralogically diagnostic absorption bands. Here we present visible (∼ 0.43-0.95 µm) and nearinfrared (∼ 0.7-2.5 µm) spectra of nine NEAs and five Mars-crossing asteroids (MCs). The YT1) as a V-type was made on the basis of its near-infrared spectrum since no visible spectrum is available for this asteroid. A mineralogical analysis was performed on six of the asteroids (those for which near-IR spectra were obtained or previously available). We found that three asteroids (241662 (2000 KO44), 19764 (2000 NF5), 138404 (2000) have mafic silicate compositions consistent with ordinary chondrites, while three others (4055 Magellan, 164121 (2003 YT1), 5407 (1992 AX)) are pyroxene-dominated basaltic achondrite assemblages. In the case of 5407 (1992 AX) we found that its basaltic surface composition contrasts its taxonomic classification as a S-type.

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Spextool: A Spectral Extraction Package for SpeX, a 0.8–5.5 Micron Cross‐Dispersed Spectrograph

Cited by 1,062 publications

References 14 publications

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

An over-massive black hole in a typical star-forming galaxy, 2 billion years after the Big Bang

Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids

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