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Start Over Author "Kemper, F." Journal monthly notices of the royal astronomical society
29 results on '"Kemper, F."'

2. LMT/AzTEC observations of Vega

Author

Marshall, J P, primary, Chavez-Dagostino, M, additional, Sanchez-Arguelles, D, additional, Matrà, L, additional, del Burgo, C, additional, Kemper, F, additional, Bertone, E, additional, Dent, W R F, additional, Vega, O, additional, Wilson, G, additional, Gómez-Ruiz, A, additional, and Montaña, A, additional

Published
2022
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3. The Nearby Evolved Stars Survey II: Constructing a volume-limited sample and first results from the James Clerk Maxwell Telescope

Author

Scicluna, P, primary, Kemper, F, additional, McDonald, I, additional, Srinivasan, S, additional, Trejo, A, additional, Wallström, S H J, additional, Wouterloot, J G A, additional, Cami, J, additional, Greaves, J, additional, He, Jinhua, additional, Hoai, D T, additional, Kim, Hyosun, additional, Jones, O C, additional, Shinnaga, H, additional, Clark, C J R, additional, Dharmawardena, T, additional, Holland, W, additional, Imai, H, additional, van Loon, J Th, additional, Menten, K M, additional, Wesson, R, additional, Chawner, H, additional, Feng, S, additional, Goldman, S, additional, Liu, F C, additional, MacIsaac, H, additional, Tang, J, additional, Zeegers, S, additional, Amada, K, additional, Antoniou, V, additional, Bemis, A, additional, Boyer, M L, additional, Chapman, S, additional, Chen, X, additional, Cho, S-H, additional, Cui, L, additional, Dell’Agli, F, additional, Friberg, P, additional, Fukaya, S, additional, Gomez, H, additional, Gong, Y, additional, Hadjara, M, additional, Haswell, C, additional, Hirano, N, additional, Hony, S, additional, Izumiura, H, additional, Jeste, M, additional, Jiang, X, additional, Kaminski, T, additional, Keaveney, N, additional, Kim, J, additional, Kraemer, K E, additional, Kuan, Y-J, additional, Lagadec, E, additional, Lee, C F, additional, Li, D, additional, Liu, S-Y, additional, Liu, T, additional, de Looze, I, additional, Lykou, F, additional, Maraston, C, additional, Marshall, J P, additional, Matsuura, M, additional, Min, C, additional, Otsuka, M, additional, Oyadomari, M, additional, Parsons, H, additional, Patel, N A, additional, Peeters, E, additional, Pham, T A, additional, Qiu, J, additional, Randall, S, additional, Rau, G, additional, Redman, M P, additional, Richards, A M S, additional, Serjeant, S, additional, Shi, C, additional, Sloan, G C, additional, Smith, M W L, additional, Suh, K-W, additional, Toalá, J A, additional, Uttenthaler, S, additional, Ventura, P, additional, Wang, B, additional, Yamamura, I, additional, Yang, T, additional, Yun, Y, additional, Zhang, F, additional, Zhang, Y, additional, Zhao, G, additional, Zhu, M, additional, and Zijlstra, A A, additional

Published
2022
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5. Nearby Evolved Stars Survey II: Constructing a volume-limited sample and first results from the James Clerk Maxwell Telescope.

Author

Scicluna, P, Kemper, F, McDonald, I, Srinivasan, S, Trejo, A, Wallström, S H J, Wouterloot, J G A, Cami, J, Greaves, J, He, Jinhua, Hoai, D T, Kim, Hyosun, Jones, O C, Shinnaga, H, Clark, C J R, Dharmawardena, T, Holland, W, Imai, H, van Loon, J Th, and Menten, K M

Subjects
*TELESCOPES, *SUBMILLIMETER astronomy, *STELLAR parallax, *DUST, *STELLAR winds, *ASYMPTOTIC giant branch stars
Abstract

The Nearby Evolved Stars Survey (NESS) is a volume-complete sample of ∼850 Galactic evolved stars within 3 kpc at (sub-)mm wavelengths, observed in the CO J  = (2–1) and (3–2) rotational lines, and the sub-mm continuum, using the James Clark Maxwell Telescope and Atacama Pathfinder Experiment. NESS consists of five tiers, based on distances and dust-production rate (DPR). We define a new metric for estimating the distances to evolved stars and compare its results to Gaia EDR3. Replicating other studies, the most-evolved, highly enshrouded objects in the Galactic Plane dominate the dust returned by our sources, and we initially estimate a total DPR of 4.7 × 10−5 M⊙ yr−1 from our sample. Our sub-mm fluxes are systematically higher and spectral indices are typically shallower than dust models typically predict. The 450/850 |$\mu$| m spectral indices are consistent with the blackbody Rayleigh–Jeans regime, suggesting a large fraction of evolved stars have unexpectedly large envelopes of cold dust. [ABSTRACT FROM AUTHOR]

Published
2022
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6. The Chemistry of Extragalactic Carbon Stars

Author

Woods, Paul, Walsh, C, Cordiner, M. A, and Kemper, F

Subjects
Astronomy, Inorganic, Organic And Physical Chemistry
Abstract

Prompted by the ongoing interest in Spitzer Infrared Spectrometer spectra of carbon stars in the Large Magellanic Cloud, we have investigated the circumstellar chemistry of carbon stars in low-metallicity environments. Consistent with observations, our models show that acetylene is particularly abundant in the inner regions of low metallicity carbon-rich asymptotic giant branch stars - more abundant than carbon monoxide. As a consequence, larger hydrocarbons have higher abundances at the metallicities of the Magellanic Clouds than in stars with solar metallicity. We also find that the oxygen and nitrogen chemistry is suppressed at lower metallicity, as expected. Finally, we calculate molecular line emission from carbon stars in the Large and Small Magellanic Cloud and find that several molecules should be readily detectable with the Atacama Large Millimeter Array at Full Science operations.

Published
2013
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7. CHIMPS2: survey description and 12CO emission in the Galactic Centre

Author

Eden, D J, primary, Moore, T J T, additional, Currie, M J, additional, Rigby, A J, additional, Rosolowsky, E, additional, Su, Y, additional, Kim, Kee-Tae, additional, Parsons, H, additional, Morata, O, additional, Chen, H-R, additional, Minamidani, T, additional, Park, Geumsook, additional, Ragan, S E, additional, Urquhart, J S, additional, Rani, R, additional, Tahani, K, additional, Billington, S J, additional, Deb, S, additional, Figura, C, additional, Fujiyoshi, T, additional, Joncas, G, additional, Liao, L W, additional, Liu, T, additional, Ma, H, additional, Tuan-Anh, P, additional, Yun, Hyeong-Sik, additional, Zhang, S, additional, Zhu, M, additional, Henshaw, J D, additional, Longmore, S N, additional, Kobayashi, M I N, additional, Thompson, M A, additional, Ao, Y, additional, Campbell-White, J, additional, Ching, T-C, additional, Chung, E J, additional, Duarte-Cabral, A, additional, Fich, M, additional, Gao, Y, additional, Graves, S F, additional, Jiang, X-J, additional, Kemper, F, additional, Kuan, Y-J, additional, Kwon, W, additional, Lee, C W, additional, Lee, J-E, additional, Liu, M, additional, Peñaloza, C H, additional, Peretto, N, additional, Phuong, N T, additional, Pineda, J E, additional, Plume, R, additional, Puspitaningrum, E, additional, Samal, M R, additional, Soam, A, additional, Sun, Y, additional, Tang, X D, additional, Traficante, A, additional, White, G J, additional, Yan, C-H, additional, Yang, A Y, additional, Yuan, J, additional, Yue, N, additional, Bemis, A, additional, Brunt, C M, additional, Chen, Z, additional, Cho, J, additional, Clark, P C, additional, Cyganowski, C J, additional, Friberg, P, additional, Fuller, G A, additional, Han, I, additional, Hoare, M G, additional, Izumi, N, additional, Kim, H-J, additional, Kim, J, additional, Kim, S, additional, Koch, E W, additional, Kuno, N, additional, Lacialle, K M, additional, Lai, S-P, additional, Lee, H, additional, Lee, Y-H, additional, Li, D L, additional, Liu, S-Y, additional, Mairs, S, additional, Pan, Z, additional, Qian, L, additional, Scicluna, P, additional, Shi, C-S, additional, Shi, H, additional, Srinivasan, S, additional, Tan, Q-H, additional, Thomas, H S, additional, Torii, K, additional, Trejo, A, additional, Umemoto, T, additional, Violino, G, additional, Wallström, S, additional, Wang, B, additional, Wu, Y, additional, Yuan, L, additional, Zhang, C, additional, Zhang, M, additional, Zhou, C, additional, and Zhou, J J, additional

Published
2020
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10. The SAGE-Spec Spitzer Legacy program: the life-cycle of dust and gas in the Large Magellanic Cloud. Point source classification – III

Author

Jones, O. C., primary, Woods, P. M., additional, Kemper, F., additional, Kraemer, K. E., additional, Sloan, G. C., additional, Srinivasan, S., additional, Oliveira, J. M., additional, van Loon, J. Th., additional, Boyer, M. L., additional, Sargent, B. A., additional, McDonald, I., additional, Meixner, M., additional, Zijlstra, A. A., additional, Ruffle, P. M. E., additional, Lagadec, E., additional, Pauly, T., additional, Sewiło, M., additional, Clayton, G. C., additional, and Volk, K., additional

Published
2017
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13. Spitzerinfrared spectrograph point source classification in the Small Magellanic Cloud

Author

Ruffle, Paul M. E., primary, Kemper, F., additional, Jones, O. C., additional, Sloan, G. C., additional, Kraemer, K. E., additional, Woods, Paul M., additional, Boyer, M. L., additional, Srinivasan, S., additional, Antoniou, V., additional, Lagadec, E., additional, Matsuura, M., additional, McDonald, I., additional, Oliveira, J. M., additional, Sargent, B. A., additional, Sewiło, M., additional, Szczerba, R., additional, van Loon, J. Th., additional, Volk,  K., additional, and Zijlstra, A. A., additional

Published
2015
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14. Molecular hydrogen emission in the interstellar medium of the Large Magellanic Cloud

Author

Naslim, N., primary, Kemper, F., additional, Madden, S. C., additional, Hony, S., additional, Chu, Y.- H., additional, Galliano, F., additional, Bot, C., additional, Yang, Y., additional, Seok, J., additional, Oliveira, J. M., additional, van Loon, J. T., additional, Meixner, M., additional, Li, A., additional, Hughes, A., additional, Gordon, K. D., additional, Otsuka, M., additional, Hirashita, H., additional, Morata, O., additional, Lebouteiller, V., additional, Indebetouw, R., additional, Srinivasan, S., additional, Bernard, J.- P., additional, and Reach, W. T., additional

Published
2014
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18. Spitzer Space Telescope spectra of post-AGB stars in the Large Magellanic Cloud – polycyclic aromatic hydrocarbons at low metallicities

Author

Matsuura, Mikako, primary, Bernard-Salas, Jeronimo, additional, Lloyd Evans, T., additional, Volk, Kevin M., additional, Hrivnak, Bruce J., additional, Sloan, G. C., additional, Chu, You-Hua, additional, Gruendl, Robert, additional, Kraemer, Kathleen E., additional, Peeters, Els, additional, Szczerba, R., additional, Wood, P. R., additional, Zijlstra, Albert A., additional, Hony, S., additional, Ita, Yoshifusa, additional, Kamath, Devika, additional, Lagadec, Eric, additional, Parker, Quentin A., additional, Reid, Warren A., additional, Shimonishi, Takashi, additional, Van Winckel, H., additional, Woods, Paul M., additional, Kemper, F., additional, Meixner, Margaret, additional, Otsuka, M., additional, Sahai, R., additional, Sargent, B. A., additional, Hora, J. L., additional, and McDonald, Iain, additional

Published
2014
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20. XSHOOTER spectroscopy of the enigmatic planetary nebula Lin49 in the Small Magellanic Cloud.

Author

Masaaki Otsuka, Kemper, F., Leal-Ferreira, M. L., Aleman, I., Bernard-Salas, J., Cami, J., Ochsendorf, B. B., Peeters, E., and Scicluna, P.

Subjects
*PLANETARY nebulae, *STELLAR photospheres, *VERY Large Telescope (Chile), *INFRARED spectroscopy, *COSMIC abundances, *SMALL magellanic cloud
Abstract

We performed a detailed spectroscopic analysis of the fullerene C60-containing planetary nebula (PN) Lin49 in the Small Magellanic Cloud (SMC) using XSHOOTER at the European Southern Observatory Very Large Telescope and the Spitzer/Infrared Spectrograph instruments. We derived nebular abundances for nine elements. We used TLUSTY to derive photospheric parameters for the central star. Lin49 is C-rich and metal-deficient PN (Z ~ 0.0006). The nebular abundances are in good agreement with asymptotic giant branch nucleosynthesis models for stars with initial mass 1.25 M⊙ and metallicity Z = 0.001. Using the TLUSTY synthetic spectrum of the central star to define the heating and ionizing source, we constructed the photoionization model with CLOUDY that matches the observed spectral energy distribution (SED) and the line fluxes in the UV to far-IR wavelength ranges simultaneously. We could not fit the ~1-5 μm SED using a model with 0.005-0.1-μm-sized graphite grains and a constant hydrogen density shell owing to the prominent near-IR excess, while at other wavelengths the model fits the observed values reasonably well. We argue that the near-IR excess might indicate either (1) the presence of very small particles in the form of small carbon clusters, small graphite sheets, or fullerene precursors, or (2) the presence of a high-density structure surrounding the central star. We found that SMC C60 PNe show a near-IR excess component to lesser or greater degree. This suggests that these C60 PNe might maintain a structure nearby their central star. [ABSTRACT FROM AUTHOR]

Published
2016
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21. On the metallicity dependence of crystalline silicates in oxygen-rich asymptotic giant branch stars and red supergiants

Author

Jones, O. C., primary, Kemper, F., additional, Sargent, B. A., additional, McDonald, I., additional, Gielen, C., additional, Woods, P. M., additional, Sloan, G. C., additional, Boyer, M. L., additional, Zijlstra, A. A., additional, Clayton, G. C., additional, Kraemer, K. E., additional, Srinivasan, S., additional, and Ruffle, P. M. E., additional

Published
2012
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24. The SAGE-Spec Spitzer Legacy programme: the life-cycle of dust and gas in the Large Magellanic Cloud - Point source classification I

Author

Woods, Paul M., primary, Oliveira, J. M., additional, Kemper, F., additional, van Loon, J. Th., additional, Sargent, B. A., additional, Matsuura, M., additional, Szczerba, R., additional, Volk, K., additional, Zijlstra, A. A., additional, Sloan, G. C., additional, Lagadec, E., additional, McDonald, I., additional, Jones, O., additional, Gorjian, V., additional, Kraemer, K. E., additional, Gielen, C., additional, Meixner, M., additional, Blum, R. D., additional, Sewiło, M., additional, Riebel, D., additional, Shiao, B., additional, Chen, C.-H. R., additional, Boyer, M. L., additional, Indebetouw, R., additional, Antoniou, V., additional, Bernard, J.-P., additional, Cohen, M., additional, Dijkstra, C., additional, Galametz, M., additional, Galliano, F., additional, Gordon, Karl D., additional, Harris, J., additional, Hony, S., additional, Hora, J. L., additional, Kawamura, A., additional, Lawton, B., additional, Leisenring, J. M., additional, Madden, S., additional, Marengo, M., additional, McGuire, C., additional, Mulia, A. J., additional, O’Halloran, B., additional, Olsen, K., additional, Paladini, R., additional, Paradis, D., additional, Reach, W. T., additional, Rubin, D., additional, Sandstrom, K., additional, Soszyński, I., additional, Speck, A. K., additional, Srinivasan, S., additional, Tielens, A. G. G. M., additional, van Aarle, E., additional, Van Dyk, S. D., additional, Van Winckel, H., additional, Vijh, Uma P., additional, Whitney, B., additional, and Wilkins, A. N., additional

Published
2010
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25. The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution

Author

Matsuura, M., primary, Barlow, M. J., additional, Zijlstra, A. A., additional, Whitelock, P. A., additional, Cioni, M.-R. L., additional, Groenewegen, M. A. T., additional, Volk, K., additional, Kemper, F., additional, Kodama, T., additional, Lagadec, E., additional, Meixner, M., additional, Sloan, G. C., additional, and Srinivasan, S., additional

Published
2009
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26. Spitzer infrared spectrograph point source classification in the Small Magellanic Cloud.

Author

Ruffle, Paul M. E., Kemper, F., Jones, O. C., Sloan, G. C., Kraemer, K. E., Woods, Paul M., Boyer, M. L., Srinivasan, S., Antoniou, V., Lagadec, E., Matsuura, M., McDonald, I., Oliveira, J. M., Sargent, B. A., Sewiło, M., Szczerba, R., van Loon, J. Th., Volk, K., and Zijlstra, A. A.

Subjects
*SMALL magellanic cloud, *CLASSIFICATION, *COSMIC dust, *STAR formation, *MAGELLANIC clouds
Abstract

The Magellanic Clouds are uniquely placed to study the stellar contribution to dust emission. Individual stars can be resolved in these systems even in the mid-infrared, and they are close enough to allow detection of infrared excess caused by dust. We have searched the Spitzer Space Telescope data archive for all Infrared Spectrograph (IRS) staring-mode observations of the Small Magellanic Cloud (SMC) and found that 209 Infrared Array Camera (IRAC) point sources within the footprint of the Surveying the Agents of Galaxy Evolution in the Small Magellanic Cloud (SAGE-SMC) Spitzer Legacy programme were targeted, within a total of 311 staring-mode observations. We classify these point sources using a decision tree method of object classification, based on infrared spectral features, continuum and spectral energy distribution shape, bolometric luminosity, cluster membership and variability information. We find 58 asymptotic giant branch (AGB) stars, 51 young stellar objects, 4 post-AGB objects, 22 red supergiants, 27 stars (of which 23 are dusty OB stars), 24 planetary nebulae (PNe), 10 Wolf-Rayet stars, 3 H II regions, 3 R Coronae Borealis stars, 1 Blue Supergiant and 6 other objects, including 2 foreground AGB stars. We use these classifications to evaluate the success of photometric classification methods reported in the literature. [ABSTRACT FROM AUTHOR]

Published
2015
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27. Molecular hydrogen emission in the interstellar medium of the Large Magellanic Cloud.

Author

Naslim, N., Kemper, F., Madden, S. C., Hony, S., Chu, Y.-H., Galliano, F., Bot, C., Yang, Y., Seok, J., Oliveira, J. M., van Loon, J. Th., Meixner, M., Li, A., Hughes, A., Gordon, K. D., Otsuka, M., Hirashita, H., Morata, O., Lebouteiller, V., and Indebetouw, R.

Subjects
*INTERSTELLAR medium, *HYDROGEN, *FIELD emission, *SPECTROGRAPHS, *PHOTODISSOCIATION, *MAGELLANIC clouds
Abstract

We present the detection and analysis of molecular hydrogen emission towards ten interstellar regions in the Large Magellanic Cloud. We examined low-resolution infrared spectral maps of 12 regions obtained with the Spitzer infrared spectrograph (IRS). The pure rotational 0-0 transitions of H2 at 28.2 and 17.1 μm are detected in the IRS spectra for 10 regions. The higher level transitions are mostly upper limit measurements except for three regions, where a 3σ detection threshold is achieved for lines at 12.2 and 8.6 μm. The excitation diagrams of the detected H2 transitions are used to determine the warm H2 gas column density and temperature. The single-temperature fits through the lower transition lines give temperatures in the range 86-137 K. The bulk of the excited H2 gas is found at these temperatures and contributes ~5-17 per cent to the total gas mass. We find a tight correlation of the H2 surface brightness with polycyclic aromatic hydrocarbon and total infrared emission, which is a clear indication of photoelectric heating in photodissociation regions. We find the excitation of H2 by this process is equally efficient in both atomic- and molecular-dominated regions. We also present the correlation of the warm H2 physical conditions with dust properties. The warm H2 mass fraction and excitation temperature show positive correlations with the average starlight intensity, again supporting H2 excitation in photodissociation regions. [ABSTRACT FROM AUTHOR]

Published
2015
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28. A Spitzer Space Telescope survey of extreme asymptotic giant branch stars in M32.

Author

Jones, O. C., McDonald, I., Rich, R. M., Kemper, F., Boyer, M. L., Zijlstra, A. A., and Bendo, G. J.

Subjects
THERMONUCLEAR reactions in stars, PROTON-proton cycle, GRAVITATIONAL collapse, SPACE telescopes, ASTRONOMICAL spectroscopy, GALAXIES, ASTRONOMICAL surveys, ASTRONOMICAL observations
Abstract

We investigate the population of cool, evolved stars in the Local Group dwarf elliptical galaxy M32, using Infrared Array Camera observations from the Spitzer Space Telescope. We construct deep mid-infrared colour-magnitude diagrams for the resolved stellar populations within 3.5 arcmin of M32's centre, and identify those stars that exhibit infrared excess. Our data are dominated by a population of luminous, dust-producing stars on the asymptotic giant branch (AGB) and extend to approximately 3 mag below the AGB tip. We detect for the first time a sizeable population of 'extreme' AGB stars, highly enshrouded by circumstellar dust and likely completely obscured at optical wavelengths. The total dust-injection rate from the extreme AGB candidates is measured to be 7.5 × 10-7 M☉ yr-1, corresponding to a gas mass-loss rate of 1.5 × 10-4 M☉ yr-1. These extreme stars may be indicative of an extended star formation epoch between 0.2 and 5 Gyr ago. [ABSTRACT FROM AUTHOR]

Published
2015
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29. The SAGE-Spec Spitzer Legacy programme: the life-cycle of dust and gas in the Large Magellanic Cloud - Point source classification I.

Author

Woods, Paul M., Oliveira, J. M., Kemper, F., van Loon, J. Th., Sargent, B. A., Matsuura, M., Szczerba, R., Volk, K., Zijlstra, A. A., Sloan, G. C., Lagadec, E., McDonald, I., Jones, O., Gorjian, V., Kraemer, K. E., Gielen, C., Meixner, M., Blum, R. D., Sewiło, M., and Riebel, D.

Subjects
COSMIC dust, MAGELLANIC clouds, INFRARED spectra, SPECTROGRAPHS, DECISION trees, SPECTRAL energy distribution, ASTRONOMICAL photometry
Abstract

We present the classification of 197 point sources observed with the Infrared Spectrograph in the SAGE-Spec Legacy programme on the Spitzer Space Telescope. We introduce a decision-tree method of object classification based on infrared spectral features, continuum and spectral energy distribution shape, bolometric luminosity, cluster membership and variability information, which is used to classify the SAGE-Spec sample of point sources. The decision tree has a broad application to mid-infrared spectroscopic surveys, where supporting photometry and variability information are available. We use these classifications to make deductions about the stellar populations of the Large Magellanic Cloud and the success of photometric classification methods. We find 90 asymptotic giant branch (AGB) stars, 29 young stellar objects, 23 post-AGB objects, 19 red supergiants, eight stellar photospheres, seven background galaxies, seven planetary nebulae, two H regions and 12 other objects, seven of which remain unclassified. [ABSTRACT FROM AUTHOR]

Published
2011
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