@article{Abbott2008,
  abstract = {Unless you're a mathematician, the chances of you reading any novels about geometry are probably slender. But if you read only two in your life, these are the ones. Taken together, they form a couple of accessible and charming explanations of geometry and physics for the curious non-mathematician. Flatland, which is also available under separate cover, was published in 1880 and imagines a two-dimensional world inhabited by sentient geometric shapes who think their planar world is all there is. But one Flatlander, a Square, discovers the existence of a third dimension and the limits of his world's assumptions about reality and comes to understand the confusing problem of higher dimensions. The book is also quite a funny satire on society and class distinctions of Victorian England. The further mathematical fantasy, Sphereland, published 60 years later, revisits the world of Flatland in time to explore the mind-bending theories created by Albert Einstein, whose work so completely altered the scientific understanding of space, time, and matter. Among Einstein's many challenges to common sense were the ideas of curved space, an expanding universe and the fact that light does not travel in a straight line. Without use of the mathematical formulae that bar most non- scientists from an understanding of Einstein's theories, Sphereland gives lay readers ways to start comprehending these confusing but fundamental questions of our reality.},
  author = {Abbott, Edwin Abbott},
  booktitle = {Dover thrift editions},
  isbn = {9780199537501},
  pages = {103},
  pmid = {26054205},
  publisher = {Oxford University Press},
  series = {Princeton Science Library},
  title = {{Flatland: A Romance of Many Dimensions}},
  volume = {Penguin cl},
  year = {2008},
}


@article{Rathborne2006a,
  author = {Rathborne, J. M. and Jackson, J. M. and Simon, R.},
  doi = {10.1086/500423},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Extinction,ISM: Clouds,ISM: Dust,Stars: Formation},
  month = {apr},
  number = {1},
  pages = {389--405},
  title = {{Infrared Dark Clouds: Precursors to Star Clusters}},
  url = {http://adsabs.harvard.edu/abs/2006ApJ...641..389R},
  volume = {641},
  year = {2006},
}


@article{Vigne2008,
  author = {{La Vigne}, MA and Vogel, SN and Ostriker, EC},
  file = {:Users/agoodman/Documents/Papers2/Files/2006La Vigne10.1086506589.pdf:pdf},
  journal = {The Astrophysical Journal},
  pages = {818--834},
  title = {{A Hubble Space Telescope archival survey of feathers in spiral galaxies}},
  url = {http://iopscience.iop.org/0004-637X/650/2/818},
  year = {2008},
}


@article{Maiz-Apellaniz2001a,
  abstract = {We have developed a method to calculate the fundamental parameters of the vertical structure of the Galaxy in the solar neighborhood from trigonometric parallaxes alone. The method takes into account Lutz-Kelker-type biases in a self-consistent way and has been applied to a sample of O-B5 stars obtained from the Hipparcos catalog. We find that the Sun is located 24.2+/-1.7 (random)+/-0.4 (systematic) pc above the Galactic plane and that the disk O-B5 stellar population is distributed with a scale height of 34.2+/-0.8 (random)+/-2.5 (systematic) pc and an integrated surface density of [1.62+/-0.04 (random)+/-0.14 (systematic)]×10-3 stars pc-2. A halo component is also detected in the distribution and constitutes at least \~{}5\% of the total O-B5 population. The O-B5 stellar population within \~{}100 pc of the Sun has an anomalous spatial distribution, with a less than average number density. This local disturbance is probably associated with the expansion of the Gould Belt. Based on data from the Hipparcos astrometry satellite.},
  author = {Ma\'{\i}z-Apell\'{a}niz, Jes\'{u}s},
  doi = {10.1086/320399},
  issn = {00046256},
  journal = {The Astronomical Journal},
  keywords = {Astrometry,Catalogs,Galaxy: Solar Neighborhood,Galaxy: Structure,Stars: Early-Type},
  month = {may},
  number = {5},
  pages = {2737--2742},
  title = {{The Spatial Distribution of O–B5 Stars in the Solar Neighborhood as Measured by [ITAL]HIPPARCOS[/ITAL][ITAL]Hipparcos[/ITAL]}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2001AJ....121.2737M},
  volume = {121},
  year = {2001},
}


@article{Blaauw1959a,
  author = {Blaauw, A. and Gum, C. S. and Pawsey, J. L. and Westerhout, G.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  month = {sep},
  pages = {702},
  title = {{Note: Definition of the New I.A.U. System of Galactic Co-Ordinates}},
  url = {http://adsabs.harvard.edu/abs/1959ApJ...130..702B},
  volume = {130},
  year = {1959},
}


@article{Corder2008,
  author = {Corder, Stuartt and Sheth, Kartik and Scoville, Nicholas Z. and Koda, Jin and Vogel, Stuart N. and Ostriker, Eve},
  doi = {10.1086/592557},
  file = {:Users/agoodman/Documents/Papers2/Files/2008Corder10.1086592557.pdf:pdf},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  month = {dec},
  number = {1},
  pages = {148--152},
  title = {{Detection of Dense Molecular Gas in Interarm Spurs in M51}},
  volume = {689},
  year = {2008},
}


@article{Drimmel2001,
  author = {Drimmel, Ronald and Spergel, David N.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Extinction,Galaxy: Disk,Galaxy: Structure,ISM: Dust,Infrared: ISM,Infrared: Stars},
  month = {jul},
  number = {1},
  pages = {181--202},
  title = {{Three‐dimensional Structure of the Milky Way Disk: The Distribution of Stars and Dust beyond 0.35 R ⊙}},
  url = {http://adsabs.harvard.edu/abs/2001ApJ...556..181D},
  volume = {556},
  year = {2001},
}


@article{Jarrett2013,
  author = {Jarrett, T. H. and Masci, F. and Tsai, C. W. and Petty, S. and Cluver, M. E. and Assef, Roberto J. and Benford, D. and Blain, a. and Bridge, C. and Donoso, E. and Eisenhardt, P. and Koribalski, B. and Lake, S. and Neill, James D. and Seibert, M. and Sheth, K. and Stanford, S. and Wright, E.},
  doi = {10.1088/0004-6256/145/1/6},
  file = {:Users/agoodman/Documents/Papers2/Files/2012Jarrett10.10880004-625614516.pdf:pdf},
  issn = {0004-6256},
  journal = {The Astronomical Journal},
  keywords = {fundamental parameters,galaxies,infrared,statistics,surveys,techniques},
  month = {jan},
  number = {1},
  pages = {6},
  title = {{Extending the Nearby Galaxy Heritage With Wise : First Results From the Wise Enhanced Resolution Galaxy Atlas}},
  volume = {145},
  year = {2013},
}


@article{Foster2012,
  abstract = {We test two different methods of using near-infrared extinction to estimate distances to dark clouds in the first quadrant of the Galaxy using large near-infrared (Two Micron All Sky Survey and UKIRT Infrared Deep Sky Survey) surveys. Very long baseline interferometry parallax measurements of masers around massive young stars provide the most direct and bias-free measurement of the distance to these dark clouds. We compare the extinction distance estimates to these maser parallax distances. We also compare these distances to kinematic distances, including recent re-calibrations of the Galactic rotation curve. The extinction distance methods agree with the maser parallax distances (within the errors) between 66\% and 100\% of the time (depending on method and input survey) and between 85\% and 100\% of the time outside of the crowded Galactic center. Although the sample size is small, extinction distance methods reproduce maser parallax distances better than kinematic distances; furthermore, extinction distance methods do not suffer from the kinematic distance ambiguity. This validation gives us confidence that these extinction methods may be extended to additional dark clouds where maser parallaxes are not available.},
  author = {Foster, Jonathan B. and Stead, Joseph J. and Benjamin, Robert A. and Hoare, Melvin G. and Jackson, James M.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: structure,ISM: clouds,dust,extinction,masers},
  month = {jun},
  number = {2},
  pages = {157},
  title = {{DISTANCES TO DARK CLOUDS: COMPARING EXTINCTION DISTANCES TO MASER PARALLAX DISTANCES}},
  url = {http://adsabs.harvard.edu/abs/2012ApJ...751..157F},
  volume = {751},
  year = {2012},
}


@article{Jackson2010,
  author = {Jackson, James M. and Finn, Susanna C. and Chambers, Edward T. and Rathborne, Jill M. and Simon, Robert},
  file = {:Users/agoodman/Documents/Papers2/Files/2010Jackson10.10882041-82057192L185.pdf:pdf},
  issn = {2041-8205},
  journal = {The Astrophysical Journal},
  keywords = {ISM: clouds,stars: formation},
  language = {en},
  month = {aug},
  number = {2},
  pages = {L185--L189},
  title = {{THE “NESSIE” NEBULA: CLUSTER FORMATION IN A FILAMENTARY INFRARED DARK CLOUD}},
  url = {http://adsabs.harvard.edu/abs/2010ApJ...719L.185J},
  volume = {719},
  year = {2010},
}


@article{McClureGriffiths2007,
  author = {McClure‐Griffiths, N. M. and Dickey, John M.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: Kinematics and Dynamics,ISM: Kinematics and Dynamics,Radio Lines: ISM},
  month = {dec},
  number = {1},
  pages = {427--438},
  title = {{Milky Way Kinematics. I. Measurements at the Subcentral Point of the Fourth Quadrant}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2007ApJ...671..427M},
  volume = {671},
  year = {2007},
}


@article{Murray2011,
  author = {Murray, Norman},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  month = {mar},
  number = {2},
  pages = {133},
  title = {{STAR FORMATION EFFICIENCIES AND LIFETIMES OF GIANT MOLECULAR CLOUDS IN THE MILKY WAY}},
  url = {http://labs.adsabs.harvard.edu/ui/abs/2011ApJ...729..133M},
  volume = {729},
  year = {2011},
}


@article{Hoffmann2012,
  author = {Hoffmann, Volker and Romeo, Alessandro B.},
  doi = {10.1111/j.1365-2966.2012.21675.x},
  file = {:Users/agoodman/Documents/Papers2/Files/2012Hoffmann10.1111j.1365-2966.2012.21675.x.pdf:pdf},
  issn = {00358711},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {1 i n t,1981,30 years after the,galaxies,instabilities,ism,kinematics and dynamics,ob-,pioneering work by larson,ro d u c,structure,t i o n,today,turbulence},
  month = {sep},
  number = {2},
  pages = {1511--1520},
  title = {{The effect of ISM turbulence on the gravitational instability of galactic discs}},
  url = {http://doi.wiley.com/10.1111/j.1365-2966.2012.21675.x},
  volume = {425},
  year = {2012},
}


@article{BlaauwA.1960,
  annote = {Galactic Pole},
  author = {{Blaauw, A.}},
  journal = {Monthly Notices of the Royal Astronomical Society},
  title = {{Optical determinations of the galactic pole}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/1960MNRAS.121..164B},
  volume = {121},
  year = {1960},
}


@article{Chen2001a,
  author = {Chen, Bing and Stoughton, Chris and Smith, J. Allyn and Uomoto, Alan and Pier, Jeffrey R. and Yanny, Brian and Ivezi\'{c}, \v{Z}eljko and York, Donald G. and Anderson, John E. and Annis, James and Brinkmann, Jon and Csabai, Istvan and Fukugita, Masataka and Hindsley, Robert and Lupton, Robert and Munn, Jeffrey A.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: Stellar Content,Galaxy: Structure},
  month = {may},
  number = {1},
  pages = {184--197},
  title = {{Stellar Population Studies with the SDSS. I. The Vertical Distribution of Stars in the Milky Way}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2001ApJ...553..184C},
  volume = {553},
  year = {2001},
}


@article{Maiz-Apellaniz2001,
  abstract = {We have developed a method to calculate the fundamental parameters of the vertical structure of the Galaxy in the solar neighborhood from trigonometric parallaxes alone. The method takes into account Lutz-Kelker-type biases in a self-consistent way and has been applied to a sample of O-B5 stars obtained from the Hipparcos catalog. We find that the Sun is located 24.2+/-1.7 (random)+/-0.4 (systematic) pc above the Galactic plane and that the disk O-B5 stellar population is distributed with a scale height of 34.2+/-0.8 (random)+/-2.5 (systematic) pc and an integrated surface density of [1.62+/-0.04 (random)+/-0.14 (systematic)]×10-3 stars pc-2. A halo component is also detected in the distribution and constitutes at least \~{}5\% of the total O-B5 population. The O-B5 stellar population within \~{}100 pc of the Sun has an anomalous spatial distribution, with a less than average number density. This local disturbance is probably associated with the expansion of the Gould Belt. Based on data from the Hipparcos astrometry satellite.},
  author = {Ma\'{\i}z-Apell\'{a}niz, Jes\'{u}s},
  issn = {00046256},
  journal = {The Astronomical Journal},
  keywords = {Astrometry,Catalogs,Galaxy: Solar Neighborhood,Galaxy: Structure,Stars: Early-Type},
  month = {may},
  number = {5},
  pages = {2737--2742},
  title = {{The Spatial Distribution of O–B5 Stars in the Solar Neighborhood as Measured by [ITAL]HIPPARCOS[/ITAL][ITAL]Hipparcos[/ITAL]}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2001AJ....121.2737M},
  volume = {121},
  year = {2001},
}


@article{Robin2003b,
  annote = {Bayesian approach near the end shows how to combine data sets.},
  author = {Robin, A. C. and Reyl�, C. and Derri�re, S. and Picaud, S.},
  doi = {10.1051/0004-6361:20031117},
  file = {:Users/agoodman/Documents/Papers2/Files/2003Robin10.10510004-636120031117.pdf:pdf},
  issn = {0004-6361},
  journal = {Astronomy and Astrophysics},
  month = {oct},
  number = {2},
  pages = {523--540},
  title = {{A synthetic view on structure and evolution of the Milky Way}},
  url = {http://labs.adsabs.harvard.edu/ui/abs/2003A\&A...409..523R},
  volume = {409},
  year = {2003},
}


@article{Brunthaler2011,
  author = {Brunthaler, A. and Reid, M.J. and Menten, K.M. and Zheng, X.-W. and Bartkiewicz, A. and Choi, Y.K. and Dame, T. and Hachisuka, K. and Immer, K. and Moellenbrock, G. and Moscadelli, L. and Rygl, K.L.J. and Sanna, A. and Sato, M. and Wu, Y. and Xu, Y. and Zhang, B.},
  file = {:Users/agoodman/Documents/Papers2/Files/2011Brunthaler.pdf:pdf},
  issn = {00046337},
  journal = {Astronomische Nachrichten},
  keywords = {Galaxy: fundamental parameters,Galaxy: kinematics and dynamics,Galaxy: structure,astrometry},
  month = {jun},
  number = {5},
  pages = {461--466},
  title = {{The Bar and Spiral Structure Legacy (BeSSeL) survey: Mapping the Milky Way with VLBI astrometry}},
  url = {http://adsabs.harvard.edu/abs/2011AN....332..461B},
  volume = {332},
  year = {2011},
}


@article{Purcell2012b,
  author = {Purcell, C. R. and Longmore, S. N. and Walsh, A. J. and Whiting, M. T. and Breen, S. L. and Britton, T. and Brooks, K. J. and Burton, M. G. and Cunningham, M. R. and Green, J. A. and Harvey-Smith, L. and Hindson, L. and Hoare, M. G. and Indermuehle, B. and Jones, P. A. and Lo, N. and Lowe, V. and Phillips, C. J. and Thompson, M. A. and Urquhart, J. S. and Voronkov, M. A. and White, G. L.},
  file = {:Users/agoodman/Documents/Papers2/Files/2012Purcell10.1111j.1365-2966.2012.21800.x-1.pdf:pdf},
  issn = {00358711},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Galaxy: structure,ISM: evolution,radio lines: ISM,stars: early-type,stars: formation,surveys},
  month = {nov},
  number = {3},
  pages = {1972--1991},
  title = {{The H 2 O Southern Galactic Plane Survey: NH 3  (1,1) and (2,2) catalogues}},
  url = {http://adsabs.harvard.edu/abs/2012MNRAS.426.1972P},
  volume = {426},
  year = {2012},
}


@article{Beuther2012a,
  abstract = {The ATLASGAL 870 $\mu$m continuum survey conducted with the APEX telescope is the first one covering the whole inner Galactic plane (60° \> l \> -60° and b \< ±1fdg5) in submillimeter (submm) continuum emission tracing the cold dust of dense and young star-forming regions. Here, we present the overall distribution of sources within our Galactic disk. The submm continuum emission is confined to a narrow range around the Galactic plane, but shifted on average by \~{}0.07 deg below the plane. Source number counts show strong enhancements toward the Galactic center, the spiral arms, and toward prominent star-forming regions. Comparing the distribution of ATLASGAL dust continuum emission to that of young intermediate- to high-mass young stellar objects (YSOs) derived from Spitzer data, we find similarities as well as differences. In particular, the distribution of submm dust continuum emission is significantly more confined to the plane than the YSO distribution (FWHM of 0.7 and 1.1 deg, corresponding to mean physical scale heights of approximately 46 and 80 pc, respectively). While this difference may partly be caused by the large extinction from the dense submm cores, gradual dispersal of stellar distributions after their birth could also contribute to this effect. Compared to other tracers of Galactic structure, the ATLASGAL data are strongly confined to a narrow latitude strip around the Galactic plane.},
  author = {Beuther, H. and Tackenberg, J. and Linz, H. and Henning, Th. and Schuller, F. and Wyrowski, F. and Schilke, P. and Menten, K. and Robitaille, T. P. and Walmsley, C. M. and Bronfman, L. and Motte, F. and Nguyen-Luong, Q. and Bontemps, S.},
  doi = {10.1088/0004-637X/747/1/43},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: structure,ISM: clouds,dust,extinction,stars: formation,stars: pre-main sequence},
  month = {mar},
  number = {1},
  pages = {43},
  title = {{GALACTIC STRUCTURE BASED ON THE ATLASGAL 870 $\mu$m SURVEY}},
  url = {http://adsabs.harvard.edu/abs/2012ApJ...747...43B},
  volume = {747},
  year = {2012},
}


@article{Blaauw1959,
  author = {Blaauw, A. and Gum, C. S. and Pawsey, J. L. and Westerhout, G.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  month = {sep},
  pages = {702},
  title = {{Note: Definition of the New I.A.U. System of Galactic Co-Ordinates}},
  url = {http://adsabs.harvard.edu/abs/1959ApJ...130..702B},
  volume = {130},
  year = {1959},
}


@article{Lee2012,
  author = {Lee, Eve J. and Murray, Norman and Rahman, Mubdi},
  doi = {10.1088/0004-637X/752/2/146},
  file = {:Users/agoodman/Documents/Papers2/Files/2012Lee10.10880004-637X7522146.pdf:pdf},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {color figures,formation,h ii regions,infrared,ism,machine-readable tables,online-only material,stars},
  month = {jun},
  number = {2},
  pages = {146},
  title = {{Milky Way Star-Forming Complexes and the Turbulent Motion of the Galaxy'S Molecular Gas}},
  volume = {752},
  year = {2012},
}


@article{Guedes2011,
  author = {Guedes, Javiera and Callegari, Simone and Madau, Piero and Mayer, Lucio},
  file = {:Users/agoodman/Documents/Papers2/Files/2011Guedes10.10880004-637X742276.pdf:pdf},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {galaxies: formation},
  language = {en},
  month = {dec},
  number = {2},
  pages = {76},
  title = {{FORMING REALISTIC LATE-TYPE SPIRALS IN A $\Lambda$CDM UNIVERSE: THE ERIS SIMULATION}},
  url = {http://adsabs.harvard.edu/abs/2011ApJ...742...76G},
  volume = {742},
  year = {2011},
}


@article{BlaauwA.1960b,
  author = {{Blaauw, A.} and {Gum, C. S.} and {Pawsey, J. L.} and {Westerhout, G.}},
  journal = {Monthly Notices of the Royal Astronomical Society},
  title = {{The new I. A. U. system of galactic coordinates (1958 revision)}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/1960MNRAS.121..123B},
  volume = {121},
  year = {1960},
}


@article{Reid2009,
  author = {Reid, M. J. and Menten, K. M. and Zheng, X. W. and Brunthaler, A. and Moscadelli, L. and Xu, Y. and Zhang, B. and Sato, M. and Honma, M. and Hirota, T. and Hachisuka, K. and Choi, Y. K. and Moellenbrock, G. A. and Bartkiewicz, A.},
  file = {:Users/agoodman/Documents/Papers 2/Files/2009Reid10.10880004-637X7001137.pdf:pdf},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: fundamental parameters,Galaxy: halo,Galaxy: kinematics and dynamics,Galaxy: structure,astrometry,stars: formation},
  month = {jul},
  number = {1},
  pages = {137--148},
  title = {{TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. VI. GALACTIC STRUCTURE, FUNDAMENTAL PARAMETERS, AND NONCIRCULAR MOTIONS}},
  url = {http://adsabs.harvard.edu/abs/2009ApJ...700..137R},
  volume = {700},
  year = {2009},
}


@article{Rathborne2006,
  author = {Rathborne, J. M. and Jackson, J. M. and Simon, R.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Extinction,ISM: Clouds,ISM: Dust,Stars: Formation},
  month = {apr},
  number = {1},
  pages = {389--405},
  title = {{Infrared Dark Clouds: Precursors to Star Clusters}},
  url = {http://adsabs.harvard.edu/abs/2006ApJ...641..389R},
  volume = {641},
  year = {2006},
}


@article{Peretto2009,
  abstract = {The majority of stars form in clusters. Therefore a comprehensive view of star formation requires understanding the initial conditions for cluster formation. The goal of our study is to shed light on the physical properties of infrared dark clouds (IRDCs) and the role they play in the formation of stellar clusters. This article, the first of a series dedicated to the study of IRDCs, describes techniques developed to establish a complete catalogue of Spitzer IRDCs in the Galaxy. We have analysed Spitzer GLIMPSE and MIPSGAL data to identify a complete sample of IRDCs in the region of Galactic longitude and latitude 10deg < |l|<65deg and |b|<1deg. From the 8micron observations we have constructed opacity maps and used a newly developed extraction algorithm to identify structures above a column density of N\_\{H2\} > 1x10\^{}\{22\} cm\^{}\{-2\}. The 24micron data are then used to characterize the star formation activity of each extracted cloud. A total of 11303 clouds have been extracted. A comparison with the existing MSX based catalogue of IRDCs shows that 80\% of these Spitzer dark clouds were previously unknown. The algorithm also extracts \~{} 20000 to 50000 fragments within these clouds, depending on detection threshold used. A first look at the MIPSGAL data indicates that between 20\% and 68\% of these IRDCs show 24micron point-like association. This new database provides an important resource for future studies aiming to understand the initial conditions of star formation in the Galaxy.},
  author = {Peretto, N. and Fuller, G. A.},
  issn = {0004-6361},
  journal = {Astronomy and Astrophysics},
  month = {oct},
  number = {1},
  pages = {405--415},
  title = {{The initial conditions of stellar protocluster formation}},
  url = {http://labs.adsabs.harvard.edu/ui/abs/2009A\&A...505..405P},
  volume = {505},
  year = {2009},
}


@article{Malhotra1994,
  abstract = {We examine the vertical structure and equilibrium of the molecular gas layer in the galactic disk, measuring its scale height and velocity dispersion as a function of Galactic radius by modeling the CO emission at the tangent points. The model takes into account emission from a large path length along the line of sight, corresponding to an interval $\backslash$Delta R \~{} 200-400 pc; and is parametrized by the scale height of the gas, the centroid in z, the rotation velocity and the velocity dispersion. This model is then fit to the \$\^{}\{12\}CO\$ survey of Knapp et al.(1985) to determine the best fit parameters. The reduced $\backslash$chi\^{}2 from fitting the models (considering only the photon statistics) range from 2 to 19. The main source of error is the `shot noise' due to the small number of clouds. Simulations using discrete molecular clouds are carried out to estimate the errors. The scale height of the molecular gas increases with radius. The velocity dispersion varies from \~{} 2 km/s to 11 km/s with a typical uncertainty of \~{}3 km/s and shows a monotonic increase with galactic radius. The midplane mass density of the disk calculated from the scale-height and velocity dispersion is consistent with the local value $\backslash$rho\_0(R\_0) of 0.2 $\backslash$msun pc\^{}\{-3\}.},
  author = {Malhotra, Sangeeta},
  file = {:Users/agoodman/Documents/Papers2/Files/1994Malhotra10.1086174677.pdf:pdf},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  month = {oct},
  pages = {687},
  title = {{The vertical equilibrium of molecular gas in the Galactic disk}},
  url = {http://labs.adsabs.harvard.edu/ui/abs/1994ApJ...433..687M},
  volume = {433},
  year = {1994},
}


@article{Dame2001,
  author = {Dame, T. M. and Hartmann, Dap and Thaddeus, P.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: Solar Neighborhood,Galaxy: Structure,ISM: Clouds,ISM: Molecules,Radio Lines: ISM,Stars: Formation},
  month = {feb},
  number = {2},
  pages = {792--813},
  title = {{The Milky Way in Molecular Clouds: A New Complete CO Survey}},
  url = {http://adsabs.harvard.edu/abs/2001ApJ...547..792D},
  volume = {547},
  year = {2001},
}


@article{Battersby,
  archiveprefix = {arXiv},
  arxivid = {arXiv:1208.4608v1},
  author = {Battersby, Cara and Bally, John},
  eprint = {arXiv:1208.4608v1},
  file = {:Users/agoodman/Documents/Papers2/Files/2012-1.pdf:pdf},
  journal = {arXiv preprint arXiv:1208.4608},
  pages = {1--2},
  title = {{An 80 pc Long Massive Molecular Filament in the Galactic Mid-Plane}},
  url = {http://arxiv.org/abs/1208.4608},
  year = {2012},
}


@article{Reid2004,
  abstract = {We report measurements with the Very Long Baseline Array (VLBA) of the position of Sgr A* with respect to two extragalactic radio sources over a period of 8 yr. The apparent proper motion of Sgr A* relative to J1745-283 is 6.379+/-0.024 mas yr-1 along a position angle of 209.60d+/-0.18d, almost entirely in the plane of the Galaxy. The effects of the orbit of the Sun around the Galactic center can account for this motion, and the residual proper motion of Sgr A* perpendicular to the plane of the Galaxy is -0.4+/-0.9 km s-1. A maximum likelihood analysis of the motion expected for a massive object within the observed Galactic center stellar cluster indicates that Sgr A* contains more than about 10\% of the \~{}4×106 Msolar deduced from stellar orbits. The intrinsic size of Sgr A*, as measured by several investigators, is less than 1 AU, and the implied mass density of \~{}1022 Msolar pc-3 is within about 3 orders of magnitude of a comparable supermassive black hole within its Schwarzschild radius. Our observations provide the first direct evidence that a compact radiative source at the center of a galaxy contains of order 106 Msolar and provides overwhelming evidence that it is in the form of a supermassive black hole. Finally, the existence of ``intermediate-mass'' black holes more massive than \~{}104 Msolar between roughly 103 and 105 AU from Sgr A* is excluded.},
  author = {Reid, M. J. and Brunthaler, A.},
  file = {:Users/agoodman/Documents/Papers2/Files/2004Reid10.1086424960.pdf:pdf},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Astrometry,Black Hole Physics,Galaxy: Center,Galaxy: Fundamental Parameters,Galaxy: Structure},
  month = {dec},
  number = {2},
  pages = {872--884},
  title = {{The Proper Motion of Sagittarius A*. II. The Mass of Sagittarius A*}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2004ApJ...616..872R},
  volume = {616},
  year = {2004},
}


@article{Malhotra1995,
  author = {Malhotra, S},
  file = {:Users/agoodman/Documents/Papers2/Files/1995Malhotra10.1086175946.pdf:pdf},
  journal = {The Astrophysical Journal},
  title = {{The Vertical Distribution and Kinematics of H i and Mass Models of the Galactic Disk}},
  year = {1995},
}


@article{Guedes2011a,
  author = {Guedes, Javiera and Callegari, Simone and Madau, Piero and Mayer, Lucio},
  doi = {10.1088/0004-637X/742/2/76},
  file = {:Users/agoodman/Documents/Papers2/Files/2011Guedes10.10880004-637X742276.pdf:pdf},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {galaxies: formation},
  language = {en},
  month = {dec},
  number = {2},
  pages = {76},
  title = {{FORMING REALISTIC LATE-TYPE SPIRALS IN A $\Lambda$CDM UNIVERSE: THE ERIS SIMULATION}},
  url = {http://adsabs.harvard.edu/abs/2011ApJ...742...76G},
  volume = {742},
  year = {2011},
}


@article{Hernandez2012,
  author = {Hernandez, Audra K. and Tan, Jonathan C. and Kainulainen, Jouni and Caselli, Paola and Butler, Michael J. and Jim\'{e}nez-Serra, Izaskun and Fontani, Francesco},
  doi = {10.1088/2041-8205/756/1/L13},
  file = {:Users/agoodman/Documents/Papers2/Files/2012Hernandez10.10882041-82057561L13-2.pdf:pdf},
  issn = {2041-8205},
  journal = {The Astrophysical Journal},
  keywords = {clouds,color figures,dust,extinction,formation,ism,online-only material,stars},
  month = {sep},
  number = {1},
  pages = {L13},
  title = {{a Virialized Filamentary Infrared Dark Cloud}},
  volume = {756},
  year = {2012},
}


@article{BlaauwA.1960c,
  annote = {Galactic Pole},
  author = {{Blaauw, A.}},
  journal = {Monthly Notices of the Royal Astronomical Society},
  title = {{Optical determinations of the galactic pole}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/1960MNRAS.121..164B},
  volume = {121},
  year = {1960},
}


@article{Purcell2012a,
  author = {Purcell, C. R. and Longmore, S. N. and Walsh, A. J. and Whiting, M. T. and Breen, S. L. and Britton, T. and Brooks, K. J. and Burton, M. G. and Cunningham, M. R. and Green, J. A. and Harvey-Smith, L. and Hindson, L. and Hoare, M. G. and Indermuehle, B. and Jones, P. A. and Lo, N. and Lowe, V. and Phillips, C. J. and Thompson, M. A. and Urquhart, J. S. and Voronkov, M. A. and White, G. L.},
  file = {:Users/agoodman/Documents/Papers 2/Files/2012Purcell.pdf:pdf},
  journal = {eprint arXiv:1207.6159},
  month = {jul},
  pages = {22},
  title = {{The H2O southern Galactic Plane Survey(HOPS): NH3 (1,1) and (2,2) catalogues}},
  url = {http://labs.adsabs.harvard.edu/ui/abs/2012arXiv1207.6159P},
  year = {2012},
}


@article{Shetty2006,
  abstract = {We investigate the formation of substructure in spiral galaxies using global MHD simulations, including gas self-gravity. Local modeling by Kim \&amp; Ostriker previously showed that self-gravity and magnetic fields cause rapid growth of overdensities in spiral arms; differential compression of gas flowing through the arms then results in the formation of sheared structures in the interarms. These sheared structures resemble features described as spurs or feathers in optical and IR observations of many spiral galaxies. Global modeling extends previous local models by including the full effects of curvilinear coordinates, a realistic log-spiral perturbation, self-gravitational contribution from five radial wavelengths of the spiral shock, and variation of density and epicyclic frequency with radius. We show that with realistic Toomre Q-values self-gravity and galactic differential rotation produce filamentary gaseous structures with kiloparsec-scale separations, regardless of the strength-or even presence-of a stellar spiral potential. However, a sufficiently strong spiral potential is required to produce true spurs, consisting of interarm structures emerging from gas concentrations in the main spiral arms. In models where Q is initially constant, filaments due to interarm self-gravity grow mainly in the outer regions, whereas true arm spurs grow only in the inner regions. For models with Q\~{}R, outer regions are intrinsically more stable, so background interarm filaments do not grow, but arm spurs can develop if the spiral potential is strong. Unlike independently growing background filaments, the orientation of arm spurs depends on galactic location. Inside corotation, spurs emanate outward, on the convex side of the arm; outside corotation, spurs grow inward, on the concave side of the arm. Based on orientation and the relation to arm clumps, it is possible to distinguish true spurs that originate as instabilities in the arms from independently growing background filaments. We measure spur spacings of \~{}3-5 times the Jeans length in the arm and arm clump masses of \~{}107 Msolar. Finally, we have also studied models without self-gravity, finding that magnetic fields suppress a purely hydrodynamic instability recently proposed by Wada \&amp; Koda as a means of growing interarm spurs and feathers. Our models also suggest that magnetic fields are important in preserving grand-design spiral structure when gas in the arms fragments via self-gravity into GMCs.},
  author = {Shetty, Rahul and Ostriker, Eve C.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxies: ISM,Galaxies: Structure,ISM: Kinematics and Dynamics,Instabilities,Magnetohydrodynamics: MHD},
  month = {aug},
  number = {2},
  pages = {997--1017},
  title = {{Global Modeling of Spur Formation in Spiral Galaxies}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2006ApJ...647..997S},
  volume = {647},
  year = {2006},
}


@article{Vallee2008a,
  author = {Vall\'{e}e, Jacques P.},
  doi = {10.1088/0004-6256/135/4/1301},
  file = {:Users/agoodman/Documents/Papers2/Files/2008Vall\'{e}e10.10880004-625613541301.pdf:pdf},
  issn = {0004-6256},
  journal = {The Astronomical Journal},
  month = {apr},
  number = {4},
  pages = {1301--1310},
  title = {{NEW VELOCIMETRY AND REVISED CARTOGRAPHY OF THE SPIRAL ARMS IN THE MILKY WAY—A CONSISTENT SYMBIOSIS}},
  url = {http://labs.adsabs.harvard.edu/ui/abs/2008AJ....135.1301V},
  volume = {135},
  year = {2008},
}


@article{Dame2011a,
  author = {Dame, T. M. and Thaddeus, P.},
  file = {:Users/agoodman/Documents/Papers2/Files/2011Dame10.10882041-82057341L24.pdf:pdf},
  issn = {2041-8205},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: structure,ISM: molecules,radio lines: ISM},
  month = {jun},
  number = {1},
  pages = {L24},
  title = {{A MOLECULAR SPIRAL ARM IN THE FAR OUTER GALAXY}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2011ApJ...734L..24D},
  volume = {734},
  year = {2011},
}


@article{BlaauwA.1960a,
  author = {{Blaauw, A.} and {Gum, C. S.} and {Pawsey, J. L.} and {Westerhout, G.}},
  journal = {Monthly Notices of the Royal Astronomical Society},
  title = {{The new I. A. U. system of galactic coordinates (1958 revision)}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/1960MNRAS.121..123B},
  volume = {121},
  year = {1960},
}


@article{Jarrett2013a,
  abstract = {The Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at mid-infrared wavelengths 3.4 $\mu$m, 4.6 $\mu$m, 12 $\mu$m, and 22 $\mu$m. The mission was primarily designed to extract point sources, leaving resolved and extended sources, for the most part, unexplored. Accordingly, we have begun a dedicated WISE Enhanced Resolution Galaxy Atlas (WERGA) project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we demonstrate the first results of the WERGA project for a sample of 17 galaxies, chosen to be of large angular size, diverse morphology, and covering a range in color, stellar mass, and star formation. It includes many well-studied galaxies, such as M 51, M 81, M 87, M 83, M 101, and IC 342. Photometry and surface brightness decomposition is carried out after special super-resolution processing, achieving spatial resolutions similar to that of Spitzer Infrared Array Camera. The enhanced resolution method is summarized in the first paper of this two-part series. In this second work, we present WISE, Spitzer, and Galaxy Evolution Explorer (GALEX) photometric and characterization measurements for the sample galaxies, combining the measurements to study the global properties. We derive star formation rates using the polycyclic aromatic hydrocarbon sensitive 12 $\mu$m (W3) fluxes, warm-dust sensitive 22 $\mu$m (W4) fluxes, and young massive-star sensitive ultraviolet (UV) fluxes. Stellar masses are estimated using the 3.4 $\mu$m (W1) and 4.6 $\mu$m (W2) measurements that trace the dominant stellar mass content. We highlight and showcase the detailed results of M 83, comparing the WISE/Spitzer results with the Australia Telescope Compact Array H I gas distribution and GALEX UV emission, tracing the evolution from gas to stars. In addition to the enhanced images, WISE's all-sky coverage provides a tremendous advantage over Spitzer for building a complete nearby galaxy catalog, tracing both stellar mass and star formation histories. We discuss the construction of a complete mid-infrared catalog of galaxies and its complementary role of studying the assembly and evolution of galaxies in the local universe.},
  author = {Jarrett, T. H. and Masci, F. and Tsai, C. W. and Petty, S. and Cluver, M. E. and Assef, Roberto J. and Benford, D. and Blain, A. and Bridge, C. and Donoso, E. and Eisenhardt, P. and Koribalski, B. and Lake, S. and Neill, James D. and Seibert, M. and Sheth, K. and Stanford, S. and Wright, E.},
  issn = {0004-6256},
  journal = {The Astronomical Journal},
  keywords = {galaxies: fundamental parameters,galaxies: statistics,infrared: galaxies,surveys,techniques: image processing},
  month = {jan},
  number = {1},
  pages = {6},
  title = {{EXTENDING THE NEARBY GALAXY HERITAGE WITH WISE : FIRST RESULTS FROM THE WISE ENHANCED RESOLUTION GALAXY ATLAS}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2013AJ....145....6J},
  volume = {145},
  year = {2013},
}


@article{Juric2008,
  author = {Juri\'{c}, Mario and Ivezi\'{c}, \v{Z}eljko and Brooks, Alyson and Lupton, Robert H. and Schlegel, David and Finkbeiner, Douglas and Padmanabhan, Nikhil and Bond, Nicholas and Sesar, Branimir and Rockosi, Constance M. and Knapp, Gillian R. and Gunn, James E. and Sumi, Takahiro and Schneider, Donald P. and Barentine, J. C. and Brewington, Howard J. and Brinkmann, J. and Fukugita, Masataka and Harvanek, Michael and Kleinman, S. J. and Krzesinski, Jurek and Long, Dan and Neilsen, Jr. and Nitta, Atsuko and Snedden, Stephanie A. and York, Donald G.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: Disk,Galaxy: Fundamental Parameters,Galaxy: Halo,Galaxy: Structure},
  month = {feb},
  number = {2},
  pages = {864--914},
  title = {{The Milky Way Tomography with SDSS. I. Stellar Number Density Distribution}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2008ApJ...673..864J},
  volume = {673},
  year = {2008},
}


@article{Lin1964,
  author = {Lin, C. C. and Shu, Frank H.},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  month = {aug},
  pages = {646},
  title = {{On the Spiral Structure of Disk Galaxies.}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/1964ApJ...140..646L},
  volume = {140},
  year = {1964},
}


@article{Wada2011,
  author = {Wada, Keiichi and Baba, Junichi and Saitoh, Takayuki R.},
  doi = {10.1088/0004-637X/735/1/1},
  file = {:Users/agoodman/Documents/Papers2/Files/2011Wada10.10880004-637X73511.pdf:pdf},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {animations,color figures,dynamics,galaxies,ism,kinematics and,kinematics and dynamics,methods,numerical,online-only material,star formation},
  month = {jul},
  number = {1},
  pages = {1},
  title = {{INTERPLAY BETWEEN STELLAR SPIRALS AND THE INTERSTELLAR MEDIUM IN GALACTIC DISKS}},
  volume = {735},
  year = {2011},
}


@article{Dobbs2011,
  author = {Dobbs, C. L. and Burkert, a. and Pringle, J. E.},
  doi = {10.1111/j.1365-2966.2011.19346.x},
  file = {:Users/agoodman/Documents/Papers2/Files/2011Dobbs10.1111j.1365-2966.2011.19346.x.pdf:pdf},
  issn = {00358711},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {clouds,evolution,hydrodynamics,ism,kinematics and dynamics},
  month = {oct},
  number = {2},
  pages = {1318--1334},
  title = {{The properties of the interstellar medium in disc galaxies with stellar feedback}},
  url = {http://doi.wiley.com/10.1111/j.1365-2966.2011.19346.x},
  volume = {417},
  year = {2011},
}


@article{Chen2001,
  author = {Chen, Bing and Stoughton, Chris and Smith, JA},
  file = {:Users/agoodman/Documents/Papers2/Files/2001Chen10.1086320647.pdf:pdf},
  journal = {The Astrophysical \ldots},
  pages = {184--197},
  title = {{Stellar Population Studies with the SDSS. I. The Vertical Distribution of Stars in the Milky Way}},
  url = {http://iopscience.iop.org/0004-637X/553/1/184},
  volume = {20},
  year = {2001},
}


@article{BarnesPeter2010,
  abstract = {We propose to combine Mopra's newly-developed Fast Mapping and pseudo-Fast-Mapping capabilities to conduct a demonstrator for a long-overdue (but previously technically forbidding) comprehensive survey of the entire southern Milky Way's molecular Interstellar Medium. In this demonstrator we will evaluate and refine our mapping strategy, in order to optimise the full survey to come. ThrUMMS' goal will be to obtain arcminute-resolution, 0.7 K sensitivity maps of 12CO and 13CO throughout the 4th quadrant. Together with other ongoing or planned surveys of the Milky Way's cold ISM, ThrUMMS' parsec-resolution maps will revolutionise our understanding of star formation, the total ecology of the ISM and its relationship with our Galaxy's stars, and the dynamics, chemistry, structure and evolution of the Milky Way itself.},
  author = {Barnes, Peter and Lo, Nadia and Muller, Erik and Cunningham, Maria and Fuller, Gary and Longmore, Steven and Brogan, Crystal and Indermuehle, Balthasar and Caselli, Paola and Molinari, Sergio and Tan, Jonathan and Lowe, Vicki and O'Dougherty, Stefan and Bania, Tom},
  journal = {ATNF proposal M566},
  keywords = {Mopra,interstellar medium in and around the Milky Way},
  title = {{ThrUMMS: the Three-mm Ultimate Mopra Milky way Survey -- A MALT110 Demonstrator}},
  url = {http://adsabs.harvard.edu/abs/2010atnf.prop.3507B},
  year = {2010},
}


@article{Tackenberg2012,
  author = {Tackenberg, J. and Beuther, H. and Henning, T. and Schuller, F. and Wienen, M. and Motte, F. and Wyrowski, F. and Bontemps, S. and Bronfman, L. and Menten, K. and Testi, L. and Lefloch, B.},
  file = {:Users/agoodman/Documents/Papers2/Files/2012Tackenberg10.10510004-6361201117412.pdf:pdf},
  issn = {0004-6361},
  journal = {Astronomy \& Astrophysics},
  keywords = {Galaxy: fundamental parameters,ISM: clouds,stars: distances,stars: formation,stars: massive,surveys},
  month = {apr},
  pages = {A113},
  title = {{Search for starless clumps in the ATLASGAL survey}},
  url = {http://adsabs.harvard.edu/abs/2012A\%26A...540A.113T},
  volume = {540},
  year = {2012},
}


@article{Malhotra1994b,
  abstract = {We examine the vertical structure and equilibrium of the molecular gas layer in the Galactic disk, measuring its scale height and velocity dispersion as a function of Galactic radius by modeling the CO emission at the tangent points. The model takes into account emission from a large path length along the line of sight, corresponding to an interval (delta R) of typically a few hundred parsecs in Galactic radius, and is parameterized by the scale height of the gas, the centroid in z, the rotation velocity, and the velocity dispersion; these parameters are assumed to be constant over the interval delta R. This model is then fitted to the (12)CO survey of Knapp, Stark, \&amp; Wilson (1985) to determine the best-fit parameters. The terminal velocity values are found to be in good agreement with those obtained from H I data. The chi-squared per degree of freedom from fitting the models (considering only the photon statistics) ranges from 2 to 19, with a median value of 6. The main source of error is found to be the 'shot noise' due to the small number of clouds. Simulations of the tangent point emission using discrete molecular clouds are carried out to estimate the errors. We use the observed radial distribution of molecular gas and the 'standard' size-line-width relation for molecular clouds in the simulations. Modeling the simulations gives values of chi-squared per degree of freedom similar to those obtained from modeling the observations. The scale height of the distribution is found to increase fairly monotonically with radius. The value of the velocity dispersion varies from approximately 2 to 11 km/s with a typical uncertainty of approximately 3 km/s. The variation in velocity dispersion is consistent with a monotonic increase with Galactic radius. The midplane mass density of the disk (rho0)(R) is calculated from the scale height and velocity dispersion (under the assumption that the velocity dispersion is isotropic) and is consistent with the local value (rho(sub0))(R0) of 0.2 solar masses/cu pc determined from stellar kinematics.},
  author = {Malhotra, Sangeeta},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {ASTRONOMICAL MODELS,CARBON MONOXIDE,COMPUTERIZED SIMULATION,DENSITY (MASS/VOLUME),EMISSION SPECTRA,EQUILIBRIUM,ERROR ANALYSIS,GALACTIC STRUCTURE,KINEMATICS,MOLECULAR GASES,RADIO ASTRONOMY,RADIO SPECTRA,SCALE HEIGHT,SKY SURVEYS (ASTRONOMY),VELOCITY DISTRIBUTION},
  month = {oct},
  pages = {687},
  title = {{The vertical equilibrium of molecular gas in the Galactic disk}},
  url = {http://adsabs.harvard.edu/abs/1994ApJ...433..687M},
  volume = {433},
  year = {1994},
}


@article{Wienen2012,
  author = {Wienen, M. and Wyrowski, F. and Schuller, F. and Menten, K. M. and Walmsley, C. M. and Bronfman, L. and Motte, F.},
  doi = {10.1051/0004-6361/201118107},
  file = {:Users/agoodman/Documents/Papers2/Files/2012Wienen10.10510004-6361201118107.pdf:pdf},
  issn = {0004-6361},
  journal = {Astronomy \& Astrophysics},
  keywords = {formation,general,ism,kinematics and dynamics,molecules,radio lines,stars,submillimeter,surveys},
  month = {aug},
  pages = {A146},
  title = {{Ammonia from cold high-mass clumps discovered in the inner Galactic disk by the ATLASGAL survey}},
  url = {http://www.aanda.org/10.1051/0004-6361/201118107},
  volume = {544},
  year = {2012},
}


@article{Chen2001b,
  author = {Chen, Bing and Stoughton, Chris and Smith, J. Allyn and Uomoto, Alan and Pier, Jeffrey R. and Yanny, Brian and Ivezi\'{c}, \v{Z}eljko and York, Donald G. and Anderson, John E. and Annis, James and Brinkmann, Jon and Csabai, Istvan and Fukugita, Masataka and Hindsley, Robert and Lupton, Robert and Munn, Jeffrey A.},
  doi = {10.1086/320647},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: Stellar Content,Galaxy: Structure},
  month = {may},
  number = {1},
  pages = {184--197},
  title = {{Stellar Population Studies with the SDSS. I. The Vertical Distribution of Stars in the Milky Way}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2001ApJ...553..184C},
  volume = {553},
  year = {2001},
}


@article{Vallee2008,
  author = {Vall\'{e}e, Jacques P.},
  file = {:Users/agoodman/Documents/Papers2/Files/2008Vall\'{e}e10.10880004-625613541301.pdf:pdf},
  issn = {0004-6256},
  journal = {The Astronomical Journal},
  month = {apr},
  number = {4},
  pages = {1301--1310},
  title = {{NEW VELOCIMETRY AND REVISED CARTOGRAPHY OF THE SPIRAL ARMS IN THE MILKY WAY—A CONSISTENT SYMBIOSIS}},
  url = {http://labs.adsabs.harvard.edu/ui/abs/2008AJ....135.1301V},
  volume = {135},
  year = {2008},
}


@article{Dame2011,
  author = {Dame, T. M. and Thaddeus, P.},
  file = {:Users/agoodman/Documents/Papers2/Files/2011Dame10.10882041-82057341L24.pdf:pdf},
  issn = {2041-8205},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: structure,ISM: molecules,radio lines: ISM},
  month = {jun},
  number = {1},
  pages = {L24},
  title = {{A MOLECULAR SPIRAL ARM IN THE FAR OUTER GALAXY}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2011ApJ...734L..24D},
  volume = {734},
  year = {2011},
}


@article{Peretto2009a,
  abstract = {The majority of stars form in clusters. Therefore a comprehensive view of star formation requires understanding the initial conditions for cluster formation. The goal of our study is to shed light on the physical properties of infrared dark clouds (IRDCs) and the role they play in the formation of stellar clusters. This article, the first of a series dedicated to the study of IRDCs, describes techniques developed to establish a complete catalogue of Spitzer IRDCs in the Galaxy. We have analysed Spitzer GLIMPSE and MIPSGAL data to identify a complete sample of IRDCs in the region of Galactic longitude and latitude 10deg < |l|<65deg and |b|<1deg. From the 8micron observations we have constructed opacity maps and used a newly developed extraction algorithm to identify structures above a column density of N\_\{H2\} > 1x10\^{}\{22\} cm\^{}\{-2\}. The 24micron data are then used to characterize the star formation activity of each extracted cloud. A total of 11303 clouds have been extracted. A comparison with the existing MSX based catalogue of IRDCs shows that 80\% of these Spitzer dark clouds were previously unknown. The algorithm also extracts \~{} 20000 to 50000 fragments within these clouds, depending on detection threshold used. A first look at the MIPSGAL data indicates that between 20\% and 68\% of these IRDCs show 24micron point-like association. This new database provides an important resource for future studies aiming to understand the initial conditions of star formation in the Galaxy.},
  archiveprefix = {arXiv},
  arxivid = {0906.3493},
  author = {Peretto, N. and Fuller, G. A.},
  doi = {10.1051/0004-6361/200912127},
  eprint = {0906.3493},
  issn = {0004-6361},
  journal = {Astronomy and Astrophysics},
  month = {oct},
  number = {1},
  pages = {405--415},
  title = {{The initial conditions of stellar protocluster formation}},
  url = {http://labs.adsabs.harvard.edu/ui/abs/2009A\&A...505..405P},
  volume = {505},
  year = {2009},
}


@article{Jarrett2012c,
  abstract = {After eight months of continuous observations, the Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at 3.4 $\mu$m, 4.6 $\mu$m, 12 $\mu$m, and 22 $\mu$m. We have begun a dedicated WISE High Resolution Galaxy Atlas project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we summarize the deconvolution techniques used to significantly improve the spatial resolution of WISE imaging, specifically designed to study the internal anatomy of nearby galaxies. As a case study, we present results for the galaxy NGC 1566, comparing the WISE enhanced-resolution image processing to that of Spitzer, Galaxy Evolution Explorer, and ground-based imaging. This is the first paper in a two-part series; results for a larger sample of nearby galaxies are presented in the second paper.},
  author = {Jarrett, T. H. and Masci, F. and Tsai, C. W. and Petty, S. and Cluver, M. and Assef, Roberto J. and Benford, D. and Blain, A. and Bridge, C. and Donoso, E. and Eisenhardt, P. and Fowler, J. and Koribalski, B. and Lake, S. and Neill, James D. and Seibert, M. and Sheth, K. and Stanford, S. and Wright, E.},
  doi = {10.1088/0004-6256/144/2/68},
  file = {:Users/agoodman/Documents/Papers2/Files/2012Jarrett10.10880004-6256144268.pdf:pdf},
  issn = {0004-6256},
  journal = {The Astronomical Journal},
  keywords = {galaxies: fundamental parameters,galaxies: statistics,infrared: galaxies,surveys,techniques: image processing},
  month = {aug},
  number = {2},
  pages = {68},
  title = {{CONSTRUCTING A WISE HIGH RESOLUTION GALAXY ATLAS}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2012AJ....144...68J},
  volume = {144},
  year = {2012},
}


@article{Juric2008a,
  author = {Juri\'{c}, Mario and Ivezi\'{c}, \v{Z}eljko and Brooks, Alyson and Lupton, Robert H. and Schlegel, David and Finkbeiner, Douglas and Padmanabhan, Nikhil and Bond, Nicholas and Sesar, Branimir and Rockosi, Constance M. and Knapp, Gillian R. and Gunn, James E. and Sumi, Takahiro and Schneider, Donald P. and Barentine, J. C. and Brewington, Howard J. and Brinkmann, J. and Fukugita, Masataka and Harvanek, Michael and Kleinman, S. J. and Krzesinski, Jurek and Long, Dan and Neilsen, Jr. and Nitta, Atsuko and Snedden, Stephanie A. and York, Donald G.},
  doi = {10.1086/523619},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: Disk,Galaxy: Fundamental Parameters,Galaxy: Halo,Galaxy: Structure},
  month = {feb},
  number = {2},
  pages = {864--914},
  title = {{The Milky Way Tomography with SDSS. I. Stellar Number Density Distribution}},
  url = {http://adsabs.harvard.edu.ezp-prod1.hul.harvard.edu/abs/2008ApJ...673..864J},
  volume = {673},
  year = {2008},
}


@ARTICLE{1960MNRAS.121..123B,
  author = {{Blaauw}, A. and {Gum}, C.~S. and {Pawsey}, J.~L. and {Westerhout}, G.},
  title = {{The new I. A. U. system of galactic coordinates (1958 revision)}},
  journal = {\mnras},
  year = {1960},
  volume = {121},
  pages = {123},
  adsurl = {http://adsabs.harvard.edu/abs/1960MNRAS.121..123B},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@ARTICLE{2012ApJ...761..189H,
  author = {{Hill}, A.~S. and {Joung}, M.~R. and {Mac Low}, M.-M. and {Benjamin}, R.~A. and {Haffner}, L.~M. and {Klingenberg}, C. and {Waagan}, K.},
  journal = {\apj},
  keywords = {Galaxy: disk, Galaxy: structure, ISM: kinematics and dynamics, ISM: structure, magnetohydrodynamics: MHD, turbulence},
  year = {2012},
  month = {dec},
  volume = {761},
  eid = {189},
  pages = {189},
  doi = {10.1088/0004-637X/761/2/189},
  adsurl = {http://adsabs.harvard.edu/abs/2012ApJ...761..189H},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@article{kauffmann2010:irdcs,
  abstract = {We present a new assessment of the ability of Infrared Dark Clouds (IRDCs) to form massive stars and clusters. This is done by comparison with an empirical mass-size threshold for massive star formation (MSF). We establish m(r)&gt;870 M sun(r/pc)1.33 as a novel approximate MSF limit, based on clouds with and without MSF. Many IRDCs, if not most, fall short of this threshold. Without significant evolution, such clouds are unlikely MSF candidates. This provides a first quantitative assessment of the small number of IRDCs evolving toward MSF. IRDCs below this limit might still form stars and clusters of up to intermediate mass, though (like, e.g., the Ophiuchus and Perseus Molecular Clouds). Nevertheless, a major fraction of the mass contained in IRDCs might reside in few 102 clouds sustaining MSF.},
  author = {Kauffmann, Jens and Pillai, Thushara},
  doi = {10.1088/2041-8205/723/1/L7},
  file = {:Users/jens/Documents/Literatur/Mendeley/Kauffmann, Pillai_2010.pdf:pdf},
  issn = {2041-8205},
  journal = {The Astrophysical Journal},
  keywords = {ISM: clouds,methods: data analysis,stars: formation},
  month = {nov},
  number = {1},
  pages = {L7--L12},
  title = {{HOW MANY INFRARED DARK CLOUDS CAN FORM MASSIVE STARS AND CLUSTERS?}},
  url = {http://adsabs.harvard.edu/abs/2010ApJ...723L...7K},
  volume = {723},
  year = {2010},
}


@article{peretto2010:irdcs-mass-density,
  abstract = {How and when the mass distribution of stars in the Galaxy is set is one of the main issues of modern astronomy. Here, we present a statistical study of mass and density distributions of infrared dark clouds (IRDCs) and fragments within them. These regions are pristine molecular gas structures and progenitors of stars and so provide insights into the initial conditions of star formation. This study makes use of an IRDC catalog, the largest sample of IRDC column density maps to date, containing a total of $\sim$11,000 IRDCs with column densities exceeding N_H_2 = 1× 10^{22} cm-2 and over 50,000 single-peaked IRDC fragments. The large number of objects constitutes an important strength of this study, allowing a detailed analysis of the completeness of the sample and so statistically robust conclusions. Using a statistical approach to assigning distances to clouds, the mass and density distributions of the clouds and the fragments within them are constructed. The mass distributions show a steepening of the slope when switching from IRDCs to fragments, in agreement with previous results of similar structures. IRDCs and fragments are divided into unbound/bound objects by assuming Larson's relation and calculating their virial parameter. IRDCs are mostly gravitationally bound, while a significant fraction of the fragments are not. The density distribution of gravitationally unbound fragments shows a steep characteristic slope such as $\Delta$N/$\Delta$log(n) vprop n -4.0±0.5, rather independent of the range of fragment mass. However, the incompleteness limit at a number density of $\sim$103 cm-3 does not allow us to exclude a potential lognormal density distribution. In contrast, gravitationally bound fragments show a characteristic density peak at n $\sim$= 104 cm-3 but the shape of the density distributions changes with the range of fragment masses. An explanation for this could be the differential dynamical evolution of the fragment density with respect to their mass as more massive fragments contract more rapidly. The IRDC properties reported here provide a representative view of the density and mass structure of dense molecular clouds before and during the earliest stages of star formation. These should serve as constraints on any theoretical or numerical model to identify the physical processes involved in the formation and evolution of structure in molecular clouds.},
  author = {Peretto, N. and Fuller, G. A.},
  doi = {10.1088/0004-637X/723/1/555},
  issn = {0004-637X},
  journal = {The Astrophysical Journal},
  keywords = {ISM: clouds,stars: formation},
  month = {nov},
  number = {1},
  pages = {555--562},
  title = {{A STATISTICAL STUDY OF THE MASS AND DENSITY STRUCTURE OF INFRARED DARK CLOUDS}},
  url = {http://adsabs.harvard.edu/abs/2010ApJ...723..555P},
  volume = {723},
  year = {2010},
}


@article{pillai2006:g11,
  author = {Pillai, T and Wyrowski, F and Menten, K.$\sim$M. and Kr\{u}gel, E},
  doi = {10.1051/0004-6361:20042145},
  file = {:Users/jens/Documents/Literatur/Mendeley/Pillai et al._2006(2).pdf:pdf},
  journal = {\aap},
  pages = {929--936},
  title = {{High mass star formation in the infrared dark cloud G11.11-0.12}},
  volume = {447},
  year = {2006},
}


@article{rathborne2007:irdc-msf,
  abstract = {Infrared dark clouds (IRDCs) are a distinct class of interstellar molecular cloud identified as dark extinction features against the bright mid-infrared Galactic background. Here we present high angular resolution millimeter continuum images obtained with the IRAM Plateau de Bure Interferometer toward four high-mass (200-1800 Msolar) IRDC cores that show evidence for active high-mass star formation (M>8 Msolar). We detect twelve bright (>7 mJy), compact (< 2, < 0.024 pc) condensations toward these cores. Two of the cores (G024.60+00.08 MM1 and G024.60+00.08 MM2) are resolved into multiple protostellar condensations, while one core (G022.35+00.41 MM1) shows two condensations. The remaining core (G024.33+00.11 MM1) contains a single, compact protostellar condensation with a very rich molecular spectrum, indicating that this is a hot molecular core associated with an early stage in the formation of a high-mass protostar. The derived gas masses for these condensations suggest that each core is forming at least one high-mass protostar (Mgas>8 Msolar), and three cores are also forming lower mass protostars (Mgas 2-5 Msolar). A comparison of the ratios of the gas masses (MG) to the Jeans masses (MJ) for IRDCs, cores, and condensations, provides broad support for the idea of hierarchical fragmentation. The close proximity of multiple protostars of disparate mass indicates that these IRDCs are in the earliest evolutionary states in the formation of stellar clusters. Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).},
  annote = {(c) 2007: The American Astronomical Society},
  author = {Rathborne, J M and Simon, R and Jackson, J M},
  doi = {10.1086/513178},
  file = {:Users/jens/Documents/Literatur/Mendeley/Rathborne, Simon, Jackson_2007.pdf:pdf},
  journal = {The Astrophysical Journal},
  keywords = {ISM: Dust,ISM: clouds,Infrared: ISM,Radio Lines: ISM,Techniques: High Anular Resolution,extinction,stars: formation},
  month = {jun},
  pages = {1082},
  title = {{The Detection of Protostellar Condensations in Infrared Dark Cloud Cores}},
  url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ApJ...662.1082R&link_type=ABSTRACT},
  volume = {662},
  year = {2007},
}


@ARTICLE{2011ApJ...734L..24D,
  author = {{Dame}, T.~M. and {Thaddeus}, P.},
  title = {{A Molecular Spiral Arm in the Far Outer Galaxy}},
  journal = {\apjl},
  archiveprefix = {arXiv},
  eprint = {1105.2523},
  primaryclass = {astro-ph.GA},
  keywords = {Galaxy: structure, ISM: molecules, radio lines: ISM},
  year = {2011},
  month = {jun},
  volume = {734},
  eid = {L24},
  pages = {L24},
  doi = {10.1088/2041-8205/734/1/L24},
  adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...734L..24D},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@ARTICLE{2013MNRAS.432..653D,
  author = {{Dobbs}, C.~L. and {Pringle}, J.~E.},
  title = {{The exciting lives of giant molecular clouds}},
  journal = {\mnras},
  archiveprefix = {arXiv},
  eprint = {1303.4995},
  primaryclass = {astro-ph.GA},
  keywords = {stars: formation, ISM: clouds, ISM: evolution, galaxies: ISM},
  year = {2013},
  month = {jun},
  volume = {432},
  pages = {653-667},
  doi = {10.1093/mnras/stt508},
  adsurl = {http://adsabs.harvard.edu/abs/2013MNRAS.432..653D},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@ARTICLE{2001ApJ...547..792D,
  author = {{Dame}, T.~M. and {Hartmann}, D. and {Thaddeus}, P.},
  title = {{The Milky Way in Molecular Clouds: A New Complete CO Survey}},
  journal = {\apj},
  eprint = {arXiv:astro-ph/0009217},
  keywords = {Galaxy: Structure, ISM: Clouds, ISM: Molecules, Radio Lines: ISM, Galaxy: Solar Neighborhood, Stars: Formation},
  year = {2001},
  month = {feb},
  volume = {547},
  pages = {792-813},
  doi = {10.1086/318388},
  adsurl = {http://adsabs.harvard.edu/abs/2001ApJ...547..792D},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@ARTICLE{2013A&ARv..21...61R,
  author = {{Rix}, H.-W. and {Bovy}, J.},
  title = {{The Milky Way's stellar disk. Mapping and modeling the Galactic disk}},
  journal = {\aapr},
  archiveprefix = {arXiv},
  eprint = {1301.3168},
  primaryclass = {astro-ph.GA},
  keywords = {Galaxy: Disk, dynamics and kinematics, formation and evolution, stellar populations, Surveys},
  year = {2013},
  month = {may},
  volume = {21},
  pages = {61},
  doi = {10.1007/s00159-013-0061-8},
  adsurl = {http://adsabs.harvard.edu/abs/2013A%26ARv..21...61R},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@ARTICLE{2012MNRAS.426.1972P,
  author = {{Purcell}, C.~R. and {Longmore}, S.~N. and {Walsh}, A.~J. and {Whiting}, M.~T. and {Breen}, S.~L. and {Britton}, T. and {Brooks}, K.~J. and {Burton}, M.~G. and {Cunningham}, M.~R. and {Green}, J.~A. and {Harvey-Smith}, L. and {Hindson}, L. and {Hoare}, M.~G. and {Indermuehle}, B. and {Jones}, P.~A. and {Lo}, N. and {Lowe}, V. and {Phillips}, C.~J. and {Thompson}, M.~A. and {Urquhart}, J.~S. and {Voronkov}, M.~A. and {White}, G.~L.},
  title = {{The H$_{2}$O Southern Galactic Plane Survey: NH$_{3}$ (1,1) and (2,2) catalogues}},
  journal = {\mnras},
  archiveprefix = {arXiv},
  eprint = {1207.6159},
  primaryclass = {astro-ph.GA},
  keywords = {surveys, stars: early-type, stars: formation, ISM: evolution, Galaxy: structure, radio lines: ISM},
  year = {2012},
  month = {nov},
  volume = {426},
  pages = {1972-1991},
  doi = {10.1111/j.1365-2966.2012.21800.x},
  adsurl = {http://adsabs.harvard.edu/abs/2012MNRAS.426.1972P},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@ARTICLE{2003PASP..115..953B,
  author = {{Benjamin}, R.~A. and {Churchwell}, E. and {Babler}, B.~L. and {Bania}, T.~M. and {Clemens}, D.~P. and {Cohen}, M. and {Dickey}, J.~M. and {Indebetouw}, R. and {Jackson}, J.~M. and {Kobulnicky}, H.~A. and {Lazarian}, A. and {Marston}, A.~P. and {Mathis}, J.~S. and {Meade}, M.~R. and {Seager}, S. and {Stolovy}, S.~R. and {Watson}, C. and {Whitney}, B.~A. and {Wolff}, M.~J. and {Wolfire}, M.~G.},
  title = {{GLIMPSE. I. An SIRTF Legacy Project to Map the Inner Galaxy}},
  journal = {\pasp},
  eprint = {astro-ph/0306274},
  keywords = {Galaxy: Stellar Content, Galaxy: Structure, infrared: general, infrared: stars, ISM: General, Surveys, Stars: General},
  year = {2003},
  month = {aug},
  volume = {115},
  pages = {953-964},
  doi = {10.1086/376696},
  adsurl = {http://adsabs.harvard.edu/abs/2003PASP..115..953B},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@ARTICLE{2009PASP..121..213C,
  author = {{Churchwell}, E. and {Babler}, B.~L. and {Meade}, M.~R. and {Whitney}, B.~A. and {Benjamin}, R. and {Indebetouw}, R. and {Cyganowski}, C. and {Robitaille}, T.~P. and {Povich}, M. and {Watson}, C. and {Bracker}, S.},
  title = {{The Spitzer/GLIMPSE Surveys: A New View of the Milky Way}},
  journal = {\pasp},
  keywords = {IYA Review},
  year = {2009},
  month = {mar},
  volume = {121},
  pages = {213-230},
  doi = {10.1086/597811},
  adsurl = {http://adsabs.harvard.edu/abs/2009PASP..121..213C},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@ARTICLE{2013A&A...559A..34L,
  author = {{Li}, G.-X. and {Wyrowski}, F. and {Menten}, K. and {Belloche}, A.},
  title = {{A 500 pc filamentary gas wisp in the disk of the Milky Way}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1310.3267},
  primaryclass = {astro-ph.GA},
  keywords = {ISM: clouds, ISM: bubbles, ISM: kinematics and dynamics, stars: formation, turbulence},
  year = {2013},
  month = {nov},
  volume = {559},
  eid = {A34},
  pages = {A34},
  doi = {10.1051/0004-6361/201322411},
  adsurl = {http://adsabs.harvard.edu/abs/2013A%26A...559A..34L},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@ARTICLE{1953ApJ...118..116C,
  author = {{Chandrasekhar}, S. and {Fermi}, E.},
  title = {{Problems of Gravitational Stability in the Presence of a Magnetic Field.}},
  journal = {\apj},
  year = {1953},
  month = {jul},
  volume = {118},
  pages = {116},
  doi = {10.1086/145732},
  adsurl = {http://adsabs.harvard.edu/abs/1953ApJ...118..116C},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}


@article{Goodman_2014,
  doi = {10.1088/0004-637x/797/1/53},
  url = {http://dx.doi.org/10.1088/0004-637X/797/1/53},
  year = {2014},
  month = {nov},
  publisher = {{IOP} Publishing},
  volume = {797},
  number = {1},
  pages = {53},
  author = {Alyssa A. Goodman and Jo{\~{a}}o Alves and Christopher N. Beaumont and Robert A. Benjamin and Michelle A. Borkin and Andreas Burkert and Thomas M. Dame and James Jackson and Jens Kauffmann and Thomas Robitaille and Rowan J. Smith},
  title = {{{THE} {BONES} {OF} {THE} {MILKY} {WAY}}},
  journal = {{ApJ}},
}