Template: https://www.inc.com/guides/2010/08/how-to-write-a-summary-business-plan.htmlDescriptionAten Engineering Inc. provides technical solutions in the areas of detection, discovery, follow-up and characterization of Near Earth Asteroids, with the goals of increasing the safety of our planet from impacting asteroids, and enabling in-space resource extraction and utilization to pave the way for Human exploration of the Solar System.Aten Engineering is currently based in the Pacific Northwest with plans to expand or relocate to LuxembourgVision StatementAten Engineering will enable the Asteroid mining industry, by providing spectroscopic typing and accurate orbits of low delta-v asteroids, using inexpensive, automated, terrestrial telescopes. 2. Vision Statement: Write a concise one- or two-paragraph vision statement, which gives your answer to the question: 'What do we want this company to become over the next five to 10 years?' 3. Mission Statement: Lay the groundwork for your 'brand promise' in a one or two paragraph description of what your company will be to its customers.  4. Values: Provide a list of three to five core principles upon which you will build the business and stick to no matter what. 5. Goals: Make a list of three to five long-term goals that translate your company's vision into specific, measurable, attainable, relevant and time-specific objectives. 6. Market research: Take the next two to three pages to briefly answer the following questions: What do you know about your industry?What do you know about your competition?Who is your target customer and what do you know about them (i.e. demographics, buying patterns)?6(a). Market differentiation: Take the next page to detail what makes your product or service unique in the market by answering questions like:What makes you different from your competition that actually matters to your target customer?What is your unique value proposition?What is your big bold brand promise?6(b). Marketing message: Based on the answers you outline above, take the next half page to explain the message you plan to communicate to your target market.6(c). Marketing mix: Use the next page or so to detail the methods you will use to deliver that message.6(d). Measurement: Follow the previous two sections with another half-page describing how you will measure the effectiveness of each of those delivery methods and, based on the results, adjust your plan accordingly.7. Sales: Take the next full page to summarize your sales plan by answering these questions:What is your overall sales process?What are the specific steps in your process?               - How are leads generated?               - How are they researched/qualified?               - How do you get in front of your customer?               - How do you close the sale?How will you achieve the optimal sales cycle?8. Operations plan: Now, take one to two pages to answer the following questions:How will you produce the product and/or deliver the service?What are the logistics?What business process will you employ?What facility, equipment, and other resource needs are involved?How will you assure and measure quality and customer satisfaction?Who are the key players?What are their backgrounds and qualifications?What are their specific roles?How will the business be organized (org. chart)?9. Personnel Plan: Use one page to describe your 'people' plan by answering questions like:What personnel are needed now to accomplish current goals?How will the number of people needed change with the growth of the business?10. Financial Plan: As noted earlier, keep the details about your financials brief, using the same narrative style you have been using throughout the plan. Then, use a footnote to alert readers that more detailed financial schedules and assumptions will exist in a separate document. To keep focused, consider telling your story by providing the following information:Start-up costs, if applicableRevenue projections with detailed assumptionsThree- to five-year cash-flow projectionsThree- to five-year balance sheet projectionsSources and uses of funds if you are raising capital11. Executive Summary: Save the beginning for the end by taking one to two pages to write a concise synopsis of the entire plan. 

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如果您正在寻找基于网页的 LaTex 编辑器,Authorea 应该是您一个不错的选择。Authorea 是一个强大的在线 LaTeX 编辑器,并拥有很多强大的功能,包括立即可用的模板,方便合作的工具,文档更改历史记录,聊天功能,自动创建参考文献,方便插入图像,链接,表格等。 Authorea 还支持多种文件格式,包括 LaTeX,HTML,Markdown 等等。索引页面的创建,导出文件为 PDF,在社交媒体上分享,支持的平台:基于网页的,支持所有主流浏览器。快速编辑,打开/关闭评论,字数统计,这些都是 Authorea 能够提供的一些主要功能。这也是为什么它能成为 LaTeX 最好的的编辑器之一,使你能方便地用你最喜欢的浏览器做 LaTeX 编辑。Authorea 使得插入数学公式,图像和表格变得非常简单。总而言之,这些功能使得 Authorea 是一款简单易用的 LaTeX 编辑工具,你不需要花费很长时间就能学会使它。主要功能:非常容易插入图像,数学公式,表格和其它对象,合作,引用文章,自动创建参考文献,评论功能,可互动的图像,可插入 Ipython/Jupyter 文本。支持的平台:基于网页的,支持所有主流浏览器。

GOAL: Create an interface that allows a users to visualize data on the history and future of global small satellite missions DATA SOURCES: Nanosatellites Database by Erik. (2016). Nanosatellite Database [Data file]. Retrieved 20 April, 2016 from http://www.nanosats.eu/. Data Hub. (2012). Countries Continents [Data file]. Retreived 13 May, 2016 from https://datahub.io/dataset/countries-continents/resource/aa08c34c-57e8-4e15-bd36-969bee26aba5 BACKGROUND: CubeSats and other small classes of satellite [1] are opening up new opportunities for space-based research. Tiny, relatively simple to build, and economical to launch, it’s not hard to see why these platforms are so appealing to people with an interest in astronomy, astrophysics, and meteorology just to name a few disciplines. Educational small satellites can even be flown for free on rockets planned for upcoming launches through NASA’s CubeSat Launch Initiative [2], making them one of the most accessible ways to prototype experimental instrumentation and study the cosmos. Unfortunately though, most small satellite data remains on private hard drives or in non-standard formats, maintained by groups that do not have the time or resources to publish and disseminate that data as there are no designated public repositories or standards to serve this function. This means that a wealth of data, which could be the foundation for new innovations and discoveries, is basically inaccessible. Worsening this problem, private companies are flying small sats with the intention of putting that data into proprietary formats and selling it back to researchers at a profit; these companies currently have little competition from the public or non-profit sector. To address these issues, myself and a multidisciplinary team at the Harvard-Smithsonian Center for Astrophysics is working to create an open source, ready-to-use, small satellite data system that will allow researchers to reduce time spent on developing ad hoc systems and invest more time in the mission and instrumentation. We’re calling it The Space Library [3]. With an open solution like the one my team is proposing, educators and the public will gain access to live space data that will be ripe for current and future citizen science projects. Researchers in astronomy and astrophysics will also be more capable of building on the experimental work that small satellites enable. On my website [4] I have hosted a few interactive data visualizations to help my team make the case for the importance of funding The Space Library. VISUALIZATIONS: I built the visualizations on my website using R (packages: dplyr, plyr, RColorBrewer) and the R API for Plotly [5], a browser-based charting library built on plotly.js. The code I used to clean the nanosatellites database data is available on GitHub here [6] along with the code I used to create the plots themselves [7]. To generate the embed codes used on this site I pushed resulting plots to my personal account on Plotly [8]. I wanted to illustrate the increasingly global impact of small satellites without creating misleading graphics that hid the drastic skew toward North America and the United States in particular; to do this I created plots that an end-user can interact with. A person can adjust the scale, zoom, subset, pan and more using the toolbar at the top of each plot, which is made visible by hovering the cursor over that area. A person can also click on the legends to deselect and select data as well as using the plots selection features to alter the presentation. I did not include in these plots any launches that did not have specified dates (TBD) or for which the launches were cancelled.

1 INSTRUCTIONS FOR CO-AUTHORS Authorlist is not final. It’s just the order in which I added to this article. Will clean up later. This is my first experience with Collaborative online article editing. We write the article here online. When we are done, I will download the LaTeX and bring it in the right form to submit. So, please edit and comment as you like and don’t worry about design and appearance. You can get started by double clicking a text block and begin editing. You can also click the Text button below a block to add new block elements. Or you can drag and drop an image right onto this text. Click the little speech bubble icon on the top right of a block to leave comments. REMEMBER TO PRESS ”SAVE AND CLOSE” AFTER EDITING A TEXT BLOCK! Delete as you see fit - it’s all in the git version control system and I can revert any edits we don’t like. You can use ”export document” on the top right of the screen to see a pdf version. If you don’t see your changes - press ”Reload” in the browser.

TYC8241 2652 1 is a young star that showed a strong mid-infrared (mid-IR, 8-25 μm) excess in all observations before 2008 CONSISTENT WITH a dusty disk. Between 2008 and 2010 the mid-IR luminosity of this system dropped dramatically by at least a factor of 30 suggesting a loss of dust mass of an order of magnitude or more. So far there is no conclusive explanation for this observational fact; possibilities include removal of disk material by stellar activity processes, a collisional cascade that rapidly grinds dust of all sizes down to where radiative blowout is effective, or a run-away accretion event spurred by the presence of gaseous material in the disk. We present new X-ray observations, optical spectroscopy, near-IR interferometry, and mid-IR photometry of this system to constrain its parameters and identify the cause of the dust mass loss. In X-rays TYC8241 2652 1 has all properties expected from a young star: Its luminosity is in the saturation regime and the abundance pattern shows enhancement of O/FE. The photospheric Hα line is filled with a weak emission feature, indicating chromospheric activity consistent THE OBSERVED LEVEL OF CORONAL EMISSION. Interferometry does not detect a companion and sets upper limits on the companion mass of 0.2, 0.35, 0.1 and 0.05 M⊙ at a distance of 0.1-4 AU, 4-6 AU, 6-11 AU, and 11-34 AU, respectively. Our mid-IR measurements, the first of the system since 2012, are consistent with the depleted dust level seen after 2009. THE NEW DATA CONFIRMS THAT STELLAR ACTIVITY IS UNLIKELY TO DESTROY THE DUST IN THE DISK AND SHOWS THAT SCENARIOS WHERE EITHER TYC8241 2652 1 HEATS THE DISK OF A BINARY COMPANION OR A POTENTIAL COMPANION HEATS THE DISK OF TYC8241 2652 1 ARE HIGLY UNLIKELY.

Internet technologies make it easier and easier to share data globally, enabling a dramatic proliferation of online “citizen science” projects. One new project, called “oldAstronomy,” is in development by the Zooniverse team, based at Chicago’s Adler Planetarium, in collaboration with the WorldWide Telescope Ambassadors program at Harvard. The goal of the project is to restore hidden metadata to images in published astronomical articles, some more than 100 years old, making the images useful to researchers. In this paper, I investigate a possible role for high school students in the oldAstronomy project. Using two focus groups, one at Milton School and one at Cambridge Ringe and Latin School, I investigate which aspects of participating in oldAstronomy would be of most interest: connections to real data? to real scientists? connecting to other students worldwide? viewing interesting images? researching a topic related to images encountered? It was explained to the focus group students, before they were surveyed, that requirements for their participation in oldAstronomy will include: digesting a scientific paper; summarizing results; and writing a summary that is understandable to the general public or participating in a more creative final project. Results show that students are very interested in working with real data and in the beauty and meaning of images. However, the results also show that students are, perhaps surprisingly, not interested in collaborating and communicating with other students, either in-person (as group work), or online. In response to the feedback from these students’ negative responses to group work, instead of a group final paper, students could benefit in a similar way with a reproduction of the peer review process. Additionally from the feedback of students, there was interest in an alternative form of final assessment. The results of our study suggest that instead of a standard write up, students can create: a 3D model of their object; a website about it; or a WorldWide Telescope tour.

The WorldWide Telescope (WWT) software environment gives explorers a Universe at their fingertips. Views of the Sky at wavelengths invisible to the human eye, virtual "3D" space travel, and seamless connections to the ever-expanding web of information online about our understanding of the Universe are available to anyone seeking to explore. WWT lets teachers and students learn in completely new, more engaging and data-rich ways, and it lets scientists communicate results, and share and contextualize data much more effectively than they ever have before. In this short article, written to commemorate the full "open-sourcing" of WorldWide Telescope software by Microsoft in 2015, we highlight just a few of the ways WWT has, and will continue to, change education, research, and scholarly communication. Detailed examples of how WorldWide Telescope is used in various settings are described at wwtstories.org.

--------------- -------------------------------------------------- NAME Alyssa A. Goodman OFFICE Astronomy Department, Harvard University Cambridge, MA 02138, 617-495-9278   HOME 485 Concord Avenue, Lexington, MA 02421 AG SITE http://cfa–www.harvard.edu/∼agoodman SEAMLESS SITE http://projects.iq.harvard.edu/seamlessastronomy ORIGIN July 1, 1962, New York, New York --------------- --------------------------------------------------

This collaborative document has been created for the panel discussion on “Rotation in massive stars” (FOE 2015), held on Thursday 6/4/2015 in Raileigh. All conference participants have been added to the document and can edit / comment / add figures (just drag&drop) / references and even LaTeX equations if needed (check the help page for more info on how to edit the document). Hopefully this will capture the essential ideas and interactions that will stem during and after the discussion. The document can be forked at any time, so that particular discussions can be taken further and potentially lead to active collaborations.

First attempt using Authorea. Just messing with text options and doing some math markdown from scratch. Trying out the citation bits and linking to GitHub. THIS IS BOLD, _This is Italic_ This is a quadratic equation:  y = x² + 2x − 3 $ y = -4(1)(-3)}}{2(1)}$ $ y = }{2}$ $ y = }{2}$ $ y = }{2}$ $ y = }{2} = 1$ $ y = }{2} = -3$

INTRODUCTION The workshop is intended to discuss ongoing and future work studying the central molecular zone of our galaxy, with a particular emphasis on the relationship between the molecular gas and star formation. The conference web page is http://eso.org/~aginsbur/ESO-CMZ-2015.html and abstracts are listed at http://eso.org/~aginsbur/abstracts.html. This document is intended to include notes from the workshop and a starting point for future work, especially observing proposals and perhaps even papers.

ECCENTRIC DISK MODEL Following the approach of Hughes, Factor, Chiang et al., we model an eccentric circumstellar disk as a series of apse-aligned ellipses. We model the mass distribution within each ellipse using a mass-on-a-wire approach. In this document, we derive the mass distribution for a single ellipse as a function of orbital position. To start, we assume that the ith ellipse we have chosen to model has a total mass of mi. The linear density of this wire, λi, with units [g/cm], is proportional to the amount of time spent in that section of the orbit. This means that the density will be largest at apoapse, when a test particle in the orbit is traveling the slowest. Conversely, the density will be smallest at periapse, when the test particle is moving fastest. The linear density is uniquely defined as a function of orbital position. We can either measure the orbital position in terms of path length along the perimeter of the ellipse, s, where s = 0 denotes periapse, or, we can measure orbital position as a function of true anomaly[1] θ, which is the same as the angle f in Meredith’s notes. Once we have defined λi, we can check that we have the right definition by integrating the linear density over the perimeter of the elliptical orbit–we should recover mi. [1] http://spiff.rit.edu/classes/phys440/lectures/ellipse/true_anomaly.gif

Recently, argued that a very long, very thin infrared dark cloud “Nessie” lies directly in the Galactic midplane and runs along the Scutum-Centaurus arm in position-position-velocity (p-p-v) space as traced by lower density CO and higher density NH₃ gas. Nessie was presented as the first “bone” of the Milky Way, an extraordinarily long, thin, high contrast filament that can be used to map our galaxy’s ”skeleton.“ We present the first evidence of additional bones in the Milky Way Galaxy, arguing that Nessie is not a curiosity but one of several filaments that could potentially trace Galactic structure. Our ten bone candidates are all long, filamentary, mid-infrared extinction features which lie parallel to, and no more than twenty parsecs from, the physical Galactic midplane. We use CO, N₂H+, HCO+ and NH₃ radial velocity data to establish the location of the candidates in p-p-v space. Of the ten filaments, six candidates also have a projected aspect ratio of ≥50: 1, run along, or extremely close to, the Scutum-Centaurus arm in p-p-v space, and exhibit no abrupt shifts in velocity. Evidence suggests that these candidates are Nessie-like filaments which mark the location of significant spiral features, with ”filament 5" replicating Nessie’s properties most strongly. As molecular spectral-line and extinction maps cover more of the sky at increasing resolution and sensitivity, we seek to find more bones in future studies, ultimately to create a global-fit to the Galaxy’s spiral arms by piecing together individual skeletal features.

ABSTRACT blah.

We propose observations of L1689B in the Ophiuchus molecular cloud (~ 125 pc). The observations will cover the Class 0 core of L1689B and the filament in which the core sits. The goal is to trace the kinematics from the filament to the core. In order to achieve this goal, we propose to observe NH_3 (1, 1) and (2, 2) line emission. By combining data from the proposed VLA observation and the GBT data planned to be taken as part of our ongoing Green Bank Ammonia Survey (GAS; GBT/15A-430), the final maps will be sensitive to spatial scales from 6 arcmin (~ 0.26 pc) to 4 arcsec (~ 500 AU). The combined (VLA+GBT) set of data will have a spectral resolution of 0.1 km/s. The spectral and angular resolution will allow us to probe fragmentation and infall motion within the core. Meanwhile, the spatial coverage will allow us to trace the any flow motion from the filament onto the core, as has been recently found in molecular line observations (for example, 12CO 1-0 and 13CO 1-0) at larger scales. Being a Class 0 (very young) core sitting on a filamentary structure with large-scale velocity gradient, L1689B appears to be an ideal place to test the theory of star formation through accretion along/across filaments.