Basically, the problem is that the NH3 abundance measured in CSEs is too large by about 10^5 or 10^6.
Myers, P. C. & Benson, P. J. 1983, ApJ, 266, 309. "Dense Cores in Dark Clouds II. NH3 Observations and Star Formation"
Pauls, T. A., Wilson, T. L., Bieging, J. H., & Martin, R. N. 1983, A&A, 124, 23. "Clumping in Orion KL: 2-Arcsecond Maps of Ammonia"
Gusten, R., Walmsley, C. M., Ungerechts, H., & Churchwell, E. 1985, A&A, 142, 381. "Temperature Determinations in Molecular Clouds of the Galactic Center"
Takano, T., Stutzki, J., Fukui, Y., & Winnewisser, G. 1986, A&A, 167, 333. "High-Angular Resolution NH3 Observations of the Bipolar Flow Source Near NGC2071"
Schilke, P., Mauersberger, R., Walmsley, C. M., & Wilson, T. L. 1990, A&A, 227, 220. "Vibrationally Excited Ammonia in the Galaxy"
Bachiller, R., Martin-Pintado, J. & Fuente, A. 1993, ApJ, 417, L45
Atmospheric
2012/12/25: Copied to Zotero, so don't need this or private library anymore...
Melsheimer, C. et.al. 2005, Radio Science, 40, RS1007 "Intercomparison of General Purpose Clear Sky Atmospheric Radiative Transfer Models for the Millimeter/Submillimeter Spectral Range" NOTE: Very good overview of atmospheric models.
Very cool measurements which are capable to mapping outgassing of this well-studied comet.
Rotational temperature from CH3OH found to be 16+-7 to 32+-8 K during period September 1999 through July 2010, consistent with a gas kinetic temperature of Tk = 25 K. Find, though, that Trot = 21+-5 K on the night-side and Trot = 31+-4 K on the day-side of the comet.
2012/12/25: Copied to Zotero, so don't need this or private library anymore...
Lai, S.-P., Girart, J. M., & Crutcher, R. M. 2003, ApJ, 598, pp. 392-399 "Interferometric Mapping of Magnetic Fields in Star-forming Regions. III. Dust and CO Polarization in DR 21(OH)"
Lai, S.-P., Velusamy, T., & Langer, W. D. 2003, ApJ, 596, pp. L239-L242 "The High Angular Resolution Measurement of Ion and Neutral Spectra as a Probe of the Magnetic Field Structure in DR 21(OH)"
Fischer, J., Sanders, D. B., Simon, M., & Solomon, P. M. 1985, ApJ, 293, 508 "High Velocity Gas Flows Associated with H2 Emission Regions - How Are They Related and What Powers Them?"
Liechti, S. & Walmsley, C. M., 1997, A&A, 321, 625-633 "Thermal Methanol Emission in the DR21 Complex. Interferometric Maps: a Comparison with Maser Emission"
Richardson, K. J., Sandell, G., Cunningham, C. T., & Davies, S. R. 1994, A&A, 286, 555-564 "DR 21(OH), a Cluster in the Making. 1: Observations in Carbon Monosulphide and Methanol"
Wilson, T. L. & Mauersberger, R. 1990, A&A, 239, 305-318 "The Internal Structure of Molecular Clouds. I - C18O, C34S and NH3 Maps of the DR 21/W 75 S Region"
Dickel, J. R., Dickel, H. R., & Wilson, W. J. 1978, ApJ, 223, 840-853 "The Detailed Structure of CO in Molecular Cloud Complexes. II. The W75-DR21 Region"
Mayer, C. H., Waak, J. A., Cheung, A. C., & Chui, M. F. 1973, ApJ, 182, L65-L69 "Ammonia in DR21(OH) and NGC2264"
Ward-Thompson, D. & Robson, E. I. 1991, MNRAS, 248, 670 "Dust Around HII Regions - III: IRAS Evidence for an Old SNR in the W75S Region?"
Wilson, T. L., Martin-Pintado, J., Gardner, F. F., & Henkel, C. 1982, A&A, 107, L10-L12 "Formaldehyde Emission From DR21(OH)"
Richardson, K. J., Sandell, G., & Krisciunas, K. 1989, A&A, 224, 199-205 "Small-Scale Structure in the DR 21/DR 21(OH) Region - A High Resolution Continuum Study at Millimetre and Submillimetre Wavelengths"
Gear, W. K., Chandler, C. J., Moore, T. J. T., Cunningham, C. T., & Duncan, W. D. 1988, MNRAS, 231, 47p "Submillimetre Observations Reveal that DR21(OH) is a Double Source"
Woody, D. P., Scott, S. L., Scoville, N. Z., Mundy, L. G., Sargent, A. I., Padin, S., Tinney, C. G., & Wilson, C. D. 1989, ApJ, 227, L41 "Interferometric Observations of 1.4mm Continuum Sources"
Padin, S., Sargent, A. I., Mundy, L. G., Scoville, N. Z., Woody, D. P., Leighton, R. B., Masson, C. R., Scott, S. L., Seling, T. V., Stapelfeldt, K. R., & Terebey, S. 1989, ApJ, 337, L45 "Interferometric C18O Observations of DR21(OH) and L1551 IRS5 at Lambda=1.4mm"
Johnston, K. J., Henkel, C., & Wilson, T. L. 1984, ApJ, 285, L85 "2(11)-2(12) Formaldehyde Emission from DR21(OH)"
Note that in practice, for deriving dust properties from the emergent SED, it may be necessary to exclude fluxes with λ lsim 100 μm due to the contribution of embedded sources as well as transiently heated very small grains (Li & Draine 2001), depending on the environment.
Least-squares SED fits to fluxes in the R-J regime, as opposed to the Wien regime, may provide accurate spectral index and density-weighted temperature, or column temperature, estimates.
In a comparison of the flux ratio and least-squares fitting methods when only three fluxes are available, we find that a direct fit with the spectral index held fixed provides more accurate estimates of the column temperature. The flux ratio method can be initially used to estimate the value of the spectral index to be held fixed for a least-squares SED fit.
Nakagawa, N. 1980, in "Interstellar Molecules", B. H. Andrew (ed.) p. 365 "Interstellar Molecules on Dust Grains"
Tielens, A. G. G. M., & Hagen, W. 1982, A&A, 114, 245 "Model Calculations of the Molecular Composition of Interstellar Grain Mantles"
Mezger, P. G., Chini, R., Kreysa, E., & Gemuend, H.-P. 1986, A&A, 160, 324 "Lambda 1300 Micron Dust Emission from Giant Molecular Clouds Close to the Galactic Center"
Schloerb, F. P., Snell, R. L., & Schwartz, P. R. 1987, ApJ, 319, 426 "1300 Micron Continuum and C18O Line Mapping of the Giant Molecular Cloud Cores in Orion, W49, and W51"
Gordon, M. A. 1987, ApJ, 326, 258 "The Continuum Spectra of Dust Complexes Associated with W3 Main, M42, W49A, and W51A"
Harrington, J. P., Monk, D. J., & Clegg, R. E. S. 1988, MNRAS, 231, 577 "Thermal Infrared Emission by Dust in the Planetary Nebula NGC 3918: A Model Analysis of IRAS Observations"
Gear, W. K., Robson, E. I., & Griffin, M. J. 1988, MNRAS, 231, 55p "Millimetre and Submillimetre Observations of the Emission from Dust in Compact HII Regions"
Weintraub, D. A., Sandell, G., & Duncan, W. D. 1989, ApJ, 340, L69 "Submillimeter Measurements of T Tauri and FU Orionis Stars"
Lis, D. C. & Leung, C. M. 1990 (preprint) "Size and Density Distribution of Very Small Dust Grains in the Barnard 5 Cloud"
Beckwith, S. V. W., Sargent, A. I., Chini, R. S., & Guesten, R. (preprint) "A Survey for Circumstellar Disks Around Young Stellar Objects"
Hildebrand, R. H. 1983, QJRAS, 24, 267-282 "The Determination of Cloud Masses and Dust Characteristics from Submillimeter Thermal Emission"
Nice analysis and derivation of vibration frequencies for NH3.
Kukolich, S. G. 1967, Phys. Rev., 156, 83
NH3(3,3) = 23870.129610 MHz for F1=4-4 hyperfine
Kukolich, S. G. & Wofsy, S. C. 1970, J. Chem. Phys., 52, 5477
NH3(4,4) = 24139.416890 MHz for F1=4-4 hyperfine
Johns, J. W. C. & McKellar, A. R. W. 1977, JMS, 64, 327 "The nu3 Fundamental Band of HDCO"
DeLucia, F., & Gordy, W. 1969, Phys. Rev., 187, 58 "Molecular-Beam Maser for the Shorter-Millimeter-Wave Region: Spectral Constants of HCN and DCN"
Bocquet, R. etal. 1996, JMS, 177, 154-159 "The Ground State Rotational Spectrum of Formaldehyde"
Isotope Ratios
Don't bother copying to Zotero.
Langer, Graedel, Frerking, & Armentrout 1984, ApJ, 277, 581 Discussion of chemical fractionation in carbon-bearing molecules.
Guesten & Ungerechts 1985, A&A, 145, 241 Discussion of carbon and nitrogen enrichment in the local disk and galactic center.
Townes & Cheung 1969, ApJL, 157, L103
Thaddeus 1972, ARAA, 10, 305
Matsakis 1979, ApJ, 234, 861
Fulkerson & Clark 1974, ApJ, 287, 723
Lucas, R. & Liszt, H. 1988 (preprint) "Interstellar Isotope Ratios from MM-Wave Molecular Absorption Spectra"
Wilson, T. L., Bieging, J., Downes, D. & Gardner, F. F. 1976, A&A, 51, 303 "Observations of the Carbon-13 Isotope of Formaldehyde"
Wannier 1980, ARAA, 18, 399 "Nuclear Abundances and Evolution of the Interstellar Medium"
Dearborn, D., Tinsley, B., & Schramm, D. 1978, ApJ, 223, 557 "On the Origin and Evolution of Isotopes of Carbon, Nitrogen, and Oxygen"
Audouze, J., Lequeux, J., & Vigroux, L. 1975, A&A, 43, 71 "Isotopes of Carbon, Nitrogen, and Oxygen as Probes of Nucleosynthesis, Stellar Mass Losses and Galactic Evolution"
Hawkins, I, Jura, M., & Meyer, D. 1985, ApJ, 294, L131 "The 12C/13C Isotope Ratio Toward Zeta Ophiuchi"
Guesten, R., Henkel, C., & Batrla, W. 1985, A&A, 149, 195 "H212CO/H213CO Ratios from Molecular Clouds Near the Galactic Center"
Zuckerman, B., Buhl, D., Palmer, P., & Snyder, L. 1974, ApJ, 189, 217 "12C/13C Abundance Ratios from Observations of Interstellar H213C18O"
Gardner, F. F. & Whiteoak, J. B. 1979, MNRAS, 188, 331 "The 12C/13C Abundance Ratio Derived from H2CO Observations of Southern Sources"
Henkel, C., Wilson, T. L., & Bieging, J. 1982, A&A, 109, 344 "Further 12C/13C Ratios from Formaldehyde: A Variation with Distance from the Galactic Center"
Gardner, F. F. & Winnewisser, G. 1975, ApJ, 197, L73 "Observations of the J=1-0 Transitions of the 13C Isotopic Species of Cyanoacetylene (HCCCN) in the Direction of Sagittarius B2"
Frerking, M. A., Wilson, R. W., Linke, R. A., & Wannier, P. G. 1980, ApJ, 240, 65 "Isotopic Abundance Ratios in Interstellar Carbon Monosulfide"
Guelin, M. & Thaddeus, P. 1979, ApJ, 227, L139 "Detection of HC18O+ in Sagittarius B2"
Henkel, C., Wilson, T. L., & Downes, D. 1979, A&A, 73, L13 "Observations of the Oxygen-18 Isotope of Formaldehyde"
Kutner, M. L, Machnik, D. E., Tucker, K. D., & Massano, W. 1982, ApJ, 254, 538 "Isotope Rations in Interstellar Formaldehyde From 6 Centimeter Observations"
Wannier, P. G., Penzias, A. A., & Jenkins, E. B. 1982, ApJ, 254, 100 "The 12CO/13CO Abundance Ratio Toward Zeta Ophiuchi"
Crutcher, R. M. & Watson, W. D. 1981, ApJ, 244, 855 "Carbon Isotope Fractionation in CO, the 13CO/12CO Ratio, and the Nature of the Diffuse Interstellar Cloud Toward Zeta Ophiuchi"
Gardner, F. F., Ribes, J. C., & Cooper, B. F. C. 1971, Astroph. Lett., 9, 181 "Detection of the 18O Isotope of Formaldehyde at 4388 MHz"
Bieging, J. H., Wilson, T. L., & Downes, D. 1981, (preprint) "Formaldehyde Absorption Measurements of Selected Galactic Molecular Clouds"
Stenholm, L. G. 1985, A&A, 149, 90 "The Accuracy of Molecular Cloud Abundances and Isotopic Ratios"
Henkel, C., Guesten, R., & Gardner, F. F. 1985, A&A, 143, 148 "12C/13C Ratios from Formaldehyde in the Inner Galactic Disk"
Wannier, P. G., Penzias, A. A., Linke, R. A., & Wilson, R. W. 1976, ApJ, 204, 26 "Isotope Abundances in Interstellar Molecular Clouds"
Watson, W. D., Anicich, V. G., & Huntress, W. T. Jr. 1976, ApJ, 205, L165 "Measurement and Significance of the Reaction 13C+ + 12CO -- 12C+ + 13CO for Alteration of the 12C/13C Ratio in Interstellar Molecules"
The chemical model used to explain the differences seen in the NH3/N2H+ ratio indicates that density along with temperature is a key parameter in determining the abundances of both NH3 and N2H+. The high density (n 106 cm-3) and temperature (T 70 K) reached in the central core allow molecules such as CO to evaporate from grain mantles. The CO desorption causes a significant destruction of N2H+ which favors the formation of HCO+.
The central core has a higher temperature and density than the western and eastern cores. Thus, a different chemistry can develop due to CO evaporation from the grain mantles. The CO desorption in the central core of AFGL5194 leads to the destruction of N2H+, so that NH3/N2H+ abundance ratio increases considerably relative to the value found in the western and eastern cores. This is supported by the fact that 13CO is not frozen out in the central core, whereas it is faintly detected in the western and eastern cores (Zhang et al. 2007). As pointed out in Section 5.2.2, collings et al. (2004) find experimental evidence that the desorption of NH3 from grain mantles takes place at a temperature of ~120 K. Therefore, since in our model we assumed a maximum temperatrue of 70 K, the high NH3/N2H+ abundance ratio in the central core is mainly a consequence of the destruction of N2H+ by CO rather than an enhancement of NH3 in the gas phase.
The high temperature reached in the central core due to the presence of hot cores seems to affect significantly the NH3/N2H+ abundance ratio, indicating that the NH3/N2H+ ratio behaves differently than in low-mass star-forming regions.
Interesting analysis of N2D+/!N2H+ ratio in Class 0, Class 0/I and Class I sources.
Find that ratio:
Decreases with increasing temperature, an indication of protostellar evolution.
Increases with increasing CO depletion factor.
Most other D/H ratio measurements from other molecules do not show this clear dependence on evolutionary state.
Hirota, T., Ikeda, M., and Yamamoto, S. 2003 preprint. "Mapping Observations of DNC and HN13C in Dark Cloud Cores"
Measured TMC1, L1512, L1544, and L63.
DNC/!HN13C distribution similar to N2H+.
H13CO+ distribution more extended thatn HN13C.
Crapsi, A., Caselli, P., Walmsley, C. M., Myers, P. C., Tafalla, M., Lee, C. W., & Bourke, T. L. 2005, ApJ, 619, 379 "Probing the Evolutionary Status of Starless Cores Through N2H+ and N2D+ Observations"
Bisschop, S. E., Fraser, H. J., Oberg, K. I., van Dischoek, E. F., and Schlemmer, S. 2006, A&A, Desorption Rates and Sticking Coefficients for CO and N2 Interstellar Ices. NOTE: More general than just for N2H+ excitation. May rule-out one of the scenarios which could explain disappearance of N2H+ in core of 04191.
Daniel, F., Cernicharo, J., Roueff, E., Gerin, M., & Dubernet, M.-L. 2007, ApJ, 667, 980 "The Excitation of N2H+ in Interstellar Molecular Clouds. II. Observations". Second part in this series. Nice analysis of hyperfine structure overlap and effects on LVG models. Includes appendices which describe the N2D+ radiative transfer models used, including rate coefficient calculations.
Physics
2012/12/26: Copied to Zotero, so don't need this or private library anymore...
Elitzur, M. 1982, Rev. Mod. Phys., 54, 1225-1260 "Physical Characteristics of Astronomical Masers"
Thompson, R. I. 1984, ApJ, 283, 165-168 "Lyman and Balmer Continuum Ionization in Zero-Age Main-Sequence Stars: Applications to the Line Excess Phenomenon"
Anthony-Twarog, B. J. 1982, AJ, 87, 1213 "The Hbeta Distance Scale for B Stars: The Orion Association"
Van Vleck, J. H. & Weisskopf, V. F. 1945, Rev. Mod. Phys., 17, 227 "On the Shape of Collision-Broadened Lines"
Planets
Exoplanets
2012/12/25: Copied to Zotero, so don't need this or private library anymore...
Very nice analysis of Mercury black body emission properties.
Analysis of use of Mercury as a millimeter calibrator source indicates +-15% accuracy at 90 GHz when using the equations they derive to account for the phase effect.
Pluto
2012/12/25: Copied to Zotero, so don't need this or private library anymore...
Stern, S. A. 1992, ARAA, 30, 185-233 "The Pluto-Charon System"
Jewitt, D. C. 1994, AJ, 107, 372-378 "Heat from Pluto"
Altenhoff, W. J., Chini, R., Hein, H., Kreysa, E., Mezger, P. G., Salter, C., & Schraml, J. B., 1988, A&A, 190, L15-L17 "First Radio Astronomical Estimate of the Temperature of Pluto"
Albrecht, R., Barbieri, C., Adorf, H.-M., Corrain, G., Gemmo, A., Greenfield, P., Hainaut, O., Hook, R. N., Tholen, D. J., Blades, J. C., & Sparks, W. B. 1994, ApJ, 435, L75-L78 "High-Resolution Imaging of the Pluto-Charon System with the Faint Object Camera of the Hubble Space Telescope"
Standish, E. M. 1994, Icarus, 108, 180-185 "Improved Ephemeris of Pluto"
Young, E. F. & Binzel, R. P. 1994, Icarus, 108, 219-224 "A New Determination of Radii and Limb Parameters for Pluto and Charon from Mutual Event Lightcurves"
Reinsch, K., Burwitz, V., and Festou, M. C. 1994, Icarus, 108, 209-218 "Albedo Maps of Pluto and Improved Physical Parameters of the Pluto-Charon System"
Titan
2012/12/25: Copied to Zotero, so don't need this or private library anymore...
Thaddeus, Vrtilek, & Gottlieb 1985, ApJL, 299, L63
Gomez-Gonzalez, J., Guelin, M., Cernicharo, J., Kahane, C., & Bogey, M. 1986, A&A, 168, L11 "Detection of Interstellar 13C Isotopes of C3H2"
Bogey & Destombes 1986, A&AL, 159, L8 "Millimeter Wave Spectrum of 13C Substitutions of Cyclopropenylidene C3H2"
Matthews, H. E., Madden, S. C., Avery, L. W., & Irvine, W. M. 1986, ApJL, 307, L69 "The C3H2 2(20)-2(11) Transition: Absorption in Cold Dark Clouds"
Madden, S. C., Irvine, W. M., & Matthews, H. E. 1986, ApJ, 311, L27 "Detections of 13C-Substituted C3H2 in Astronomical Sources"
Green, S., DeFrees, D. J., & McLean, A. D. 1987, ApJS, 65, 175 "Collisional Excitation of Interstellar Cyclopropenylidene"
Vrtilek, J. M., Gottlieb, C. A., & Thaddeus, P. 1987, ApJ, 314, 716 "Laboratory and Astronomical Spectroscopy of C3H2, The First Interstellar Organic Ring"
Gerin, M., Wootten, H. A., Combes, F., Boulanger, F., Peters, W. L. II, Kuiper, T. B. H., Encrenaz, P. J., & Bogey, M. 1987, A&A, 173, L1 "Deuterated C3H2 as a Clue to Deterium Chemistry"
Adams, N. G. & Smith, D. 1987, ApJ, 317, L25 "On the Synthesis of c-C3H2 in Interstellar Clouds"
Cox, P., Walmsley, C. M., & Guesten, R. 1989, A&A, 209, 382 "C3H2 Observations in Dense Dark Clouds"
Madden, S. C., Irvine, W. M., Matthews, H. E., Friberg, P., & Swade, D. A. 1989, AJ, 97, 1403 "A Survey of Cyclopropenylidene (C3H2) in Galactic Sources"
Bell, M. B., Feldman, P. A., Matthews, H. E., & Avery, L. A., preprint "Detection of Deuterated Cyclopropenylidene (C3HD) in TMC-1"
Matthews & Irvine, ApJL, 298, L61
c-C3H
Don't bother copying to Zotero.
Yamamoto, S., Saito, S., Ohishi, M., Suzuki, H., Ishikawa, S.-I., Kaifu, N., & Murakami, A. 1987, ApJL, 322, L55 "Laboratory and Astronomical Detection of the Cyclic C3H Radical"
Mangum, J. G. & Wootten, A. 1990, A&A, 239, 319 "Observations of the Cyclic C3H Radical in the Interstellar Medium"
Supernova Remnants
2012/12/25: Copied to Zotero, so don't need this or private library anymore...
The reference for a complete and up-to-date understanding of the star formation process.
Spitzer key programme study of Serpens, Perseus, Ophiuchus, Lupus, and Chamaeleon.
After careful background galaxy removal, estimate that their YSO sample is complete to 90% down to a luminosity integrated from 1 to 30 micron of 0.05 Lsolar and 50% complete down to 0.01 Lsolar for their most distant cloud (Serpens at 260 pc).
Total of 1024 YSOs in their final sampl, which is an order-of-magnitude increase over previous samples.
For distinguishing Class 0 from Class I, find that Lbol/Lsubmm may be a better distinguisher than Tbol. This is likely due to the fact that acretion onto the YSO is not steady (appears to be episodic).
Note that early estimates of the Class 0 lifetime (about 0.01 Myr), based on a small number of Class 0s in Oph, are too small by a factor of 50. More like 0.16 Myr.
Best estimate for the Class II lifetime is 2+-1 Myr (though this should probably be viewed as a half-life rather than an actual lifetime for all Class II objects).
Minimum mean density of prestellar cores is about 2X10^4 cm^(-3), which suggests a lifetime of about 0.5+-0.1(+-0.3) Myr, where the uncertainty in parentheses includes the range over different clouds.
The distribution of sources are broadly consistent with a picture in which most stars form in clusters or groups and disperse at a rate reflecting the cloud turbulence.
Suggest some solar system formation scenarios based on this study.
For Serpens, which is the most centrally-condensed cluster:
NH3 emission lines suggest low turbulence.
13CO 1-0 emission lines suggest high turbulence (largest line widths of the sample).
Collisions of dense cores, at the stage that they observe them, are not dominant.
Monnier, J. D. & Millan-Gabet 2002, ApJ, in press "On the Interferometric Sizes of Young Stellar Objects"
Lee, C.-F., Mundy, L. G., Stone, J. M., & Ostriker, E. C. 2002, ApJ, 576, 294 "CO Outflows from Young Stellar Objects"
Mueller, K. E., Shirley, Y. L., Evans, N. J. II, & Jacobson, H. R. 2002, ApJS, 143, 469 "The Physical Conditions for Massive Star Formation: Dust Continuum Maps and Modeling"
Shirley, Y. L., Evans, N. J. II, & Rawlings, J. M. C. 2002, ApJ, 575, 337 "Tracing the Mass During Low-Mass Star Formation. III. Models of the Submillimeter Dust Continuum Emission from Class 0 Protostars"
Young, C. H., Shirley, Y. L., Evans, N. J. II, & Rawlings, J. M. C. 2002, ApJS, 145, 111 "Tracing the Mass During Low-Mass Star Formation. IV. Observations and Modeling of the Submillimeter Continuum Emission from Class I Protostars"
Lee, C.-F., Ho, P. T. P., & White, S. 2005, ApJ 619, 948. "Molecular Line Observations of IRAM 04191-1522"
Lee, J.-E., Bergin, E. A., & Evans, N. J. II, 2005, astroph 0408091 "Evolution of Chemistry and Molecular Line Profile During Protostellar Collapse"
Andrews, S. M. & Williams, J. P. 2004, ApJ, 619, L175-L178 "Submillimeter Array Observations of Disks in the SR 24 Multiple Star System"
Rodríguez, L. F., Loinard L., D'Alessio, P., Wilner, D. J., & Ho, P. T. P. 2005, ApJ, 621, L133-L136 "IRAS 16293-2422B: A Compact, Possibly Isolated Protoplanetary Disk in a Class 0 Object"
Stark, R. et.al. 2004, ApJ, 608, 341-364 "Probing the Early Stages of Low-Mass Star Formation in LDN1689N: Dust and Water in IRAS 16293-2422A, B, and E"
Belloche, A. & Andre, P. 2004, A&A, 419, L35-L38 "Disappearance of N2H+ from the Gas Phase in the Class 0 Protostar IRAM04191"
Schoier, F. L., Jorgensen, J. K., van Dishoeck, E. F., & Blake, G. A. 2004, A&A, 418, 185-202 "On the Origin of H2CO Abundance Enhancements in Low-Mass Protostars"
Tafalla, M., Myers, P. C., Caselli, P., & Walmsley, C. M. 2004, A&A, 416, 191-212 "On the Internal Structure of Starless Cores. I. Physical Conditions and the Distribution of CO, CS, N2H+, and NH3 in L1498 and L1517B"
Maret, S. et.al. 2004, A&A, 416, 577-594 "The H2CO Abundance in the Inner Warm Regions of Low Mass Protostellar Envelopes"
Cabrit, S. & Bertout, C. 1992, A&A, 261, 274-284 "CO Line Formation in Bipolar Outflows: III. The Energetics of Molecular Flows and Ionized Winds"
Testi, L., Natta, A., Oliva, E., D'Antona, F., Comeron, F., Baffa, C., Comoretto, G., & Gennari, S. 2002, ApJ, 571, L155-L159 "A Young Very Low Mass Object Surrounded by Warm Dust"
Kamazaki, T., Saito, M., Hirano, N., Umemoto, T., & Kawabe, R. 2003, ApJ, 584, 357-367 "Molecular Outflow Search in the Rho Ophiuchi A and B2 Regions"
Shirley, Y. L., Evans, N. J. II, & Rawlings, J. M. C. 2002, ApJ, 575, 337-353 "Tracing the Mass During Low-Mass Star Formation. III. Models of the Submillimeter Dust Continuum Emission from Class 0 Protostars"
Young, C. H., Shirley, Y. L., Evans, N. J. II, & Rawlings, J. M. C. 2002, ApJS, 145, 111-145 "Tracing the Mass during Low-Mass Star Formation. IV. Observations and Modeling of the Submillimeter Continuum Emission from Class I Protostars"
Harvey, D. W. A., Wilner, D. J., Myers, P. C., & Tafalla, M. 2003, ApJ, 597, 424-433 "Inner Structure of Starless Core L694-2 Derived from Millimeter-Wave Interferometry"
Evans, N. J., II 1991, in "Frontiers of Stellar Evolution" (A92-51676 22-90). San Francisco, CA, Astronomical Society of the Pacific, 1991, p. 45-95 "Star formation - Observations"
Ward-Thompson, D. 1994, in "Clouds, Cores, and Low Mass Stars", Astronomical Society of the Pacific Conference Series, volume 65; Proceedings of the 4th Haystack Observatory Conference; Haystack Observatory; Westford; Massachusetts; 18-20 May; 1994; San Francisco: Astronomical Society of the Pacific (ASP); copyright 1994; edited by Dan P. Clemens and Richard Barvainis, p.207 "First Submm Continuum Maps of Pre-Protostellar Cores"
Various Authors, "Clouds, Cores, and Low Mass Stars", Astronomical Society of the Pacific Conference Series, volume 65; Proceedings of the 4th Haystack Observatory Conference; Haystack Observatory; Westford; Massachusetts; 18-20 May; 1994; San Francisco: Astronomical Society of the Pacific (ASP); copyright 1994; edited by Dan P. Clemens and Richard Barvainis, p.207
Evans, N. J., II, 1999, ARAA, 37, 311-362 "Physical Conditions in Regions of Star Formation"
Bachiller, R. 1996, ARAA, 34, 111-154 "Bipolar Molecular Outflows from Young Stars and Protostars"
Genzel, R. 1991, in "The Physics of Star Formation and Early Stellar Evolution", pp 155-219, ed. C. J. Lada and N. D. Kylafis (Kluwer) "Physical Conditions and Heating/Cooling Processes in High Mass Star Formation Regions"
Find that VLA NH3(2,2) emission is more resolved-out than VLA NH3(1,1), indicating that the kinetic temperature of the more extended (presumably lower density) material in the L1544 core is higher than in the compact nucleus.
PdBI CO 2-1 and 1mm and 3mm continuum measurements detecting no emission, suggesting that the emission was resolved-out.
Find kinetic temperature gradient running from 6 K in the core to 11 K in the more extended (outer) regions.
See no freeze-out of NH3 or NH2D up to densities greater than 10^6 cm^(-3).
Derive a more peaked density structure (due to the lower Tk in the core) with a factor-of-two larger central density than that derived in the past.
Measure the CO2 15.2 micron bending mode toward 50 embedded YSOs, taken mainly from the c2d survey.
Measure average solid CO2:H2O = 0.32+-0.02 in low-mass YSOs, significantly higher than that found in quiescent molecular clouds and massive star formation regions.
The formation of pure CO2 via segregation from the H2O-rich dust mantles in these regions appears to require relatively high kinetic temperatures (>~ 50 K) in these regions.
Measure the CH4 7.7 micron bending mode toward 52 embedded YSOs, taken mainly from the c2d survey.
Find that the inferred solid CH4 abundances are consistent with models where CH4 is formed through sequential hydrogenation of C on grain surfaces.
The equal or higher abundances of CH4 toward low-mass YSOs compared with high-mass objects and the correlation studies support the sequential hydrogenation of C on grain surfaces as the CH4 formation pathway, but not the two competing theories: formation from CH3OH and formation in gas phase with subsequent freezeout.
Serpens
2012/12/27: Copied to Zotero, so don't need this or private library anymore...
Eiroa, C., Djupvik, A. A., and Casali, M. M. 2008, Handbook of Star Forming Regions, Vol. II, p. 1, Astronomical Society of the Pacific, Reipurth ed., "The Serpens Molecular Cloud"
Excellent general overview of Serpens with what appears to me to be a complete listing of the observed properties of the Serpens molecular cloud.
Wolf-Chase, G. A., Barsony, M., Wootten, H. A., Ward-Thompson, D., Lowrance, P. J., Kastner, J. H., & McMullin, J. P. 1998, ApJ, 501, L193-L198 "The Protostellar Origin of a CS Outflow in S68N"
Hogerheijde, M. R., van Dishoeck, E. F., Salverda, J. M., and Blake, G. A. 1999, ApJ, 513, 350-369 "Envelope Structure of Deeply Embedded Young Stellar Objects in the Serpens Molecular Cloud"
Davis, C. J., Matthews, H. E., Ray, T. P., Dent, W. R. F., and Richer, J. S. 1999, MNRAS, 309, 141-152 "A Burst of Outflows from the Serpens Cloud Core: Wide-Field Submillimetre Continuum, CO J=2-1 and Optical Observations"
McMullin, J. P., Mundy, L. G., Blake, G. A., Wilking, B. A., Mangum, J. G., and Latter, W. B. 2000, ApJ, 536, 845-856 "A Spectral Line Study of Serpens S68 FIRS1 Region"
Testi, L. & Sargent, A. I. 2000, ApJ, 508, L91-L94 "Star Formation in Clusters: A Survey of Compact Millimeter-Wave Sources in the Serpens Core"
Casali, M. M., Eiroa, C., & Duncan, W. D. 1993, A&A, 275, 195 "A Second Phase of Star Formation in the Serpens Core"
Eiroa, C., Torrelles, J. M., Curiel, S., & Djupvik, A. A. 2005, astro-ph/0506054 (2 Jun 2005)
Perseus
2012/12/27: Copied to Zotero, so don't need this or private library anymore...
Measured dust and CO in IRS43, L1689SNO2, SR24, and Elias 30 with OVRO.
Detect CO 1-0 in SR24 (recall that Andrews and Williams did not detect CO emission in this object).
Find that only primary is detected in dust, which is different from what is detected from younger protostellar binaries. This suggests that binary evolution diminishes the mass of secondary protostellar disks.
Taurus
2012/12/27: Copied to Zotero, so don't need this or private library anymore...
Find that a better model of the spiral arms in the Milky Way removes a previously-found correlation between ice ages and transit of the solar system across spiral arms.
Technical References
General
2012/12/27: Copied to Zotero, but still will need to keep these as many are not online...
Greve, A., and Morris, D. 2005, IEEE Trans. on Antennas and Propagation. "Repetitive Radio Reflector Surface Deformations"
Greve, A., Bremer, M., Penalver, J., Raffin, P., and Morris, D. 2005, IEEE Trans. on Antennas and Propagation, 53, 851-860 "Improvement of the IRAM 30m Telescope from Temperature Measurements and Finite-Element Calculations"
Butler, B. J. 2003, ALMA Memo 479 "Requirements for Subreflector and Feed Positioning for ALMA Antennas"
Ruze, J. 1967, Microwave Journal, December 1968 (based on CAMROC Technical Memo No. 19, dated 10 February 1967, Cambridge Radio Observatory Committee), "Feed Support Blockage Loss in Parabolic Antennas"
Lamb, J. W. & Olver, A. D. 1986, IEE Proceedings, 133, pt. H, 43, "Blockage Due to Subreflector Supports in Large Radiotelescope Antennas"
Kerr, A. R. 1998, MMA Memo 236 "Suggestions for Revised Definitions of Noise Quantities, Including Quantum Effects"
Kerr, A. R., Feldman, M. J., & Pan, S.-K. 1996, MMA Memo 161 "Receiver Noise Temperature, the Quantum Noise Limit, and the Role of the Zero-Point Fluctuations"
Kooi, J. W., Chattopadhyay, G., Thielman, M., Phillips, T. G., & Schieder, R. 2000, International Journal of Infrared and Millimeter Waves, 21, 689 "Noise Stability of SIS Receivers"
Cohen, M., Carbon, D. F., Welch, W. J., Lim, T., Schulz, B., McMurry, A. D., Forster, J. R., & Goorvitch, D. 2005, ApJ, 129, 2836 "Far-Infrared and Millimeter Continuum Studies of K Giants: alpha Bootis and alpha Tauri"
Butler, B. 1999, VLBA Test Memo 62 "Simulation of Some Types of Holography Errors for VLBA Antennas"
Measure 143 GHz flux stability of Neptune and Uranus.
Note that WMAP has constrained Mars, Uranus, and Neptune brightness to an accuracy of ~1%, ~3%, and ~8%, respectively, by calibrating them relative to the CMB.
Find that Uranus and Neptune behave as ideal sources for flux calibration at 143 GHz, with no evidence for temporal brightness variations.
For Uranus, these results are in contrast to the lower frequency measurements at 8.6 and 90 GHz where a flux variation of ~0.5%/year has been measured. This result is not necessarily inconsistent with the lack of flux variation at 143 GHz, though, as the higher frequency measurements probe higher altitudes in the Uranus atmosphere.
Measure decrease of ~10% (2 sigma; observational error 5%) in Uranus Tb(90 GHz) from 1985-2005 as function of sub-earth point (SEP) latitude, indicating that the south polar region is significantly brighter at millimeter wavelengths than the equatorial regions.
No variation of Neptune's Tb(90 GHz) observed to within the 8% observational error.