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News Article | June 28, 2017

CINCINNATI--(BUSINESS WIRE)--Astronomer, a data engineering platform, closed $3.5M in new financing, led by Wireframe Ventures in San Francisco and CincyTech in Cincinnati. Other investors include Frontline Ventures (UK), Grand Ventures, Drummond Road, Core Network, M25 Group, with debt financing participation from Silicon Valley Bank. For high-growth startups to Fortune 500 enterprises, data analytics has become a critical requirement for winning in today’s business environment. However, most companies struggle to build this capability, due to the complexity of accessing, organizing and managing large amounts of data. According to Forbes, even data science teams spend up to 80% of their time simply preparing data before it’s ready for high-value business analysis. Astronomer’s data engineering platform automates this heavy lifting through the release of a library of reusable connectors and pipelines “recipes” that seamlessly collect and route data from any source, like Salesforce or Google Analytics, to any destination, like Redshift or MySQL, in an enterprise. The result is dramatically less time wasted on data preparation and routing and spent, instead, on extracting valuable business insight from their data and realizing untapped revenue potential. “Data engineering, which includes accessing and preparing data for analysis, takes up the vast majority of a business analyst’s time. We constantly hear the same complaint—not only is this incredibly inefficient, but the opportunity cost is tremendous. If organizations implement a focused, iterative data engineering effort, they’d free up their people to extract insights that impact the bottom line,” said Ry Walker, Co-founder and CEO of Astronomer. “Despite major advancements in big data technology platforms over the last decade, data engineering continues to be a manual and highly labor-intensive barrier to wider adoption. Astronomer’s platform can greatly streamline this complex upfront work, enabling a much wider set of enterprises to fully leverage the power of data science to help drive business performance,” said Harsh Patel, Managing Partner of Wireframe Ventures. Astronomer plans to use this financing to grow its product and engineering teams and expand sales efforts. Astronomer customers include P&G, Everything But The House (EBTH) and Roadtrippers, along with many other enterprise, mid-market and startup organizations. Astronomer is a data engineering platform that collects and prepares data for analytics and data science and is accessible to an entire organization. Founded in Cincinnati, Ohio in 2015, the current team of 50 is comprised of top data engineers and software developers from organizations like Facebook, Oracle, E&Y and the FBI.

Kim C.,Seoul National University | Kim C.,West Virginia University | Perera B.B.P.,West Virginia University | Perera B.B.P.,University of Manchester | And 2 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2015

The Double Pulsar (PSR J0737-3039) is the only neutron star-neutron star (NS-NS) binary in which both NSs have been detectable as radio pulsars. The Double Pulsar has been assumed to dominate the Galactic NS-NS binary merger rate Rg among all known systems, solely based on the properties of the first-born, recycled pulsar (PSR J0737-3039A, or A) with an assumption for the beaming correction factor of 6. In this work, we carefully correct observational biases for the second-born, non-recycled pulsar (PSR J0737-0737B, or B) and estimate the contribution from the Double Pulsar on Rg using constraints available from both A and B. Observational constraints from the B pulsar favour a small beaming correction factor for A (~2), which is consistent with a bipolar model. Considering known NS-NS binaries with the best observational constraints, including both A and B, we obtain Rg = 21-14+28 Myr-1 at 95 per cent confidence from our reference model. We expect the detection rate of gravitational waves from NS-NS inspirals for the advanced ground-based gravitational-wave detectors is to be 8-5+10 yr-1 at 95 per cent confidence. Within several years, gravitational-wave detections relevant to NS-NS inspirals will provide us useful information to improve pulsar population models. © 2015 The Authors.

Rees L.,Astronomer
Environmental Law and Management | Year: 2013

Population trends beyond 2050 will depend on what people now in their teens and 20s decide about the number and spacing of their children. Hundreds of millions of women are denied such a choice. There is a valuable organization called the 'Optimum Population Trust' which highlights the problems of overpopulation. And there is the key issue of the discount rate. Commercial decisions apply a discount that assigns minimal importance to what happens at the end of the century. But surely we should not value the grandchildren's welfare less than the own. It is ironic that there is only one area of policy where we do implicitly apply a zero discount rate: radioactive waste disposal, where people talk with a straight face about whether the repository would be safe for ten thousand years. Geoengineering would be an utter political nightmare: not all nations would want to adjust the thermostat the same way. Very elaborate climatic modeling would be needed in order to calculate the regional impacts of such an intervention.

Prochter G.E.,University of California at Santa Cruz | Prochaska J.X.,University of California at Santa Cruz | O'Meara J.M.,Saint Michael's College | O'Meara J.M.,Astronomer | And 2 more authors.
Astrophysical Journal | Year: 2010

We present an absorption line analysis of the Lyman limit system (LLS) at z ≈ 3.55 in our Magellan/MIKE spectrum of PKS2000 - 330. Our analysis of the Lyman limit and full H I Lyman series constrains the total H I column density of the LLS (N HI = 1018.0 ± 0.25 cm-2 for b HI ≥ 20 km s-1) and also the N HI values of the velocity subsystems comprising the absorber. We measure ionic column densities for metal-line transitions associated with the subsystems and use these values to constrain the ionization state (>90% ionized) and relative abundances of the gas. We find an order of magnitude dispersion in the metallicities of the subsystems, marking the first detailed analysis of metallicity variations in an optically thick absorber. The results indicate that metals are not well mixed within the gas surrounding high z galaxies. Assuming a single-phase photoionization model, we also derive an N H-weighted metallicity, 〈[Si/H]〉 = -1.66 ±0.25, which matches the mean metallicity in the neutral interstellar medium in high z damped Lyα systems (DLAs). Because the line density of LLSs is over 10× higher than the DLAs, we propose that the former dominate the metal mass-density at z ∼ 3 and that these metals reside in the galaxy/intergalactic medium interface. Considerations of a multi-phase model do not qualitatively change these conclusions. Finally, we comment on an anomalously large O0/Si + ratio in the LLS that suggests an ionizing radiation field dominated by soft UV sources (e.g., a starburst galaxy). Additional abundance analysis is performed on the super-LLS systems at z ≈ 3.19. © 2010. The American Astronomical Society.

Mansfield R.L.,Astronomer
Advances in the Astronautical Sciences | Year: 2014

This paper presents a method of initial orbit determination (IOD) for use with short arcs of deep-space, angles-only observations. The method is then used to determine the Earth flyby path of the asteroid 2012 DA14 on 2013 February 15, as an extreme example. (The asteroid was inbound and 150-116 Earth radii distant from Earth during the time span of the observations.) The solution is obtained in geocentric coordinates, rather than heliocentric, to emphasize the significance, for Earth, of close-Earth asteroid encounters. Being founded in the work of Paul Herget, the method uses all of the available observations in the arc, not just three, as with classical IOD methods. But when only three suitably-spaced observations are available, it provides an exact, two-body fit. The method is modular with respect to the Lambert solution. It is therefore a schema or framework for preliminary orbit determination, in that any of the Lambert solutions of Gauss, Battin, Gooding, or der could be incorporated. But for the asteroid example at hand, a Lambert solution attributable Gauss, with some modifications, is used to illustrate the method.

Belton M.J.S.,Belton Space Exploration Initiatives | Belton M.J.S.,Astronomer
Icarus | Year: 2015

I show that the size-distribution of small scattered-disk trans-neptunian objects when derived from the observed size-distribution of Jupiter Family comets (JFCs) and other observational constraints implies that a large percentage (94-97%) of newly arrived active comets within a range of 0.2-15.4km effective radius must physically disrupt, i.e., macroscopically disintegrate, within their median dynamical lifetime. Additional observational constraints include the numbers of dormant and active nuclei in the near-Earth object (NEO) population and the slope of their size distributions. I show that the cumulative power-law slope (-2.86 to -3.15) of the scattered-disk TNO hot population between 0.2 and 15.4km effective radius is only weakly dependent on the size-dependence of the otherwise unknown disruption mechanism. Evidently, as JFC nuclei from the scattered disk evolve into the inner Solar System only a fraction achieve dormancy while the vast majority of small nuclei (e.g., primarily those with effective radius <2km) break-up. The percentage disruption rate appears to be comparable with that of the dynamically distinct Oort cloud and Halley type comets (Levison, H.F., Morbidelli, A., Dones, L., Jedicke, R., Wiegert, P.A., Bottke Jr., W.F. [2002]. Science 296, 2212-2215) suggesting that all types of comet nuclei may have similar structural characteristics even though they may have different source regions and thermal histories. The typical disruption rate for a 1km radius active nucleus is ~5×10-5disruptions/year and the dormancy rate is typically 3 times less. We also estimate that average fragmentation rates range from 0.01 to 0.04events/year/comet, somewhat above the lower limit of 0.01events/year/comet observed by Chen and Jewitt (Chen, J., Jewitt, D.C. [1994]. Icarus 108, 265-271). © 2014 Elsevier Inc.

Crocker A.F.,University of Massachusetts Amherst | Crocker A.F.,University of Oxford | Bureau M.,University of Oxford | Young L.M.,New Mexico Institute of Mining and Technology | And 2 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2011

We present new mm interferometric and optical integral-field unit (IFU) observations and construct a sample of 12 elliptical (E) and lenticular (S0) galaxies with molecular gas which have both CO and optical maps. The galaxies contain 2 × 107 to 5 × 109 M of molecular gas distributed primarily in central discs or rings (radii 0.5-4 kpc). The molecular gas distributions are always coincident with distributions of optically obscuring dust that reveal tightly wound spiral structures in many cases. The ionized gas always approximately corotates with the molecular gas, evidencing a link between these two gas components, yet star formation is not always the dominant ionization source. The galaxies with less molecular gas tend to have [O iii]/Hβ emission-line ratios at high values not expected for star formation. Most E/S0s with molecular gas have young or intermediate-age stellar populations based on optical colours, ultraviolet colours and absorption linestrengths. The few that appear purely old lie close to the limit where such populations would be undetectable based on the mass fractions of expected young to observed old stars. The 8 μm polycyclic aromatic hydrocarbon (PAH) and 24 μm emission yield similar star formation rate (SFR) estimates of E/S0s, but the total infrared overpredicts the rate due to a contribution to dust heating from older stars. The radio-far-infrared relation also has much more scatter than for other star-forming galaxies. However, despite these biases and additional scatter, the derived star formation rates locate the E/S0 galaxies within the large range of the Schmidt-Kennicutt and constant efficiency star formation laws. Thus, the star formation process in E/S0s is not overwhelmingly different than in other star-forming galaxies, although one of the more reliable tracers (24 μm) points to a possible lower star formation efficiency at a given gas surface density. © 2010 The Authors. Journal compilation © 2010 RAS.

Eilek J.A.,New Mexico Institute of Mining and Technology | Eilek J.A.,Astronomer
New Journal of Physics | Year: 2014

In this paper I present dynamic models of the radio source Centaurus A, and critique possible models of in situ particle reacceleration (ISR) within the radio lobes. The radio and γ-ray data require neither homogeneous plasma nor quasi-equipartition between the plasma and magnetic field; inhomogeneous models containing both high-field and low-field regions are equally likely. Cen A cannot be as young as the radiative lifetimes of its relativistic electrons, which range from a few to several tens of Myr. Two classes of dynamic models - flow driven and magnetically driven - are consistent with current observations; each requires Cen A to be on the order of a Gyr old. Thus, ongoing ISR must be occuring within the radio source. Alfven-wave ISR is probably occuring throughout the source, and may be responsible for maintaining the γ-ray-loud electrons. This is likely to be supplemented by shock or reconnection ISR, which maintains the radio-loud electrons in high-field regions. © 2014 IOP Publishing Ltd and Deutsche Physikalische Gesellschaft.

Anderson L.D.,West Virginia University | Anderson L.D.,Astronomer | Bania T.M.,Boston University | Balser D.S.,U.S. National Radio Astronomy Observatory | And 5 more authors.
Astrophysical Journal, Supplement Series | Year: 2014

Using data from the all-sky Wide-Field Infrared Survey Explorer (WISE) satellite, we made a catalog of over 8000 Galactic H II regions and H II region candidates by searching for their characteristic mid-infrared (MIR) morphology. WISE has sufficient sensitivity to detect the MIR emission from H II regions located anywhere in the Galactic disk. We believe this is the most complete catalog yet of regions forming massive stars in the Milky Way. Of the ∼8000 cataloged sources, ∼1500 have measured radio recombination line (RRL) or Hα emission, and are thus known to be H II regions. This sample improves on previous efforts by resolving H II region complexes into multiple sources and by removing duplicate entries. There are ∼2500 candidate H II regions in the catalog that are spatially coincident with radio continuum emission. Our group's previous RRL studies show that ∼95% of such targets are H II regions. We find that ∼500 of these candidates are also positionally associated with known H II region complexes, so the probability of their being bona fide H II regions is even higher. At the sensitivity limits of existing surveys, ∼4000 catalog sources show no radio continuum emission. Using data from the literature, we find distances for ∼1500 catalog sources, and molecular velocities for ∼1500H II region candidates. © 2014. The American Astronomical Society. All rights reserved.

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