This is much better on iPad than ShareLaTeX.It nicely supports the arrow keys as expected.

IntroductionThe format of this template follows a typical journal publication with an introduction, results and conclusion. Examples of an equation, list and citation are also included. The purpose of the introductionMost academic introductions follow an ‘inverted pyramid’ structure: they start broad and narrow down to a specific thesis or research question. The introduction should reveal:some broad knowledge of the overall topicreferences to related and prior work in the field of investigationsuccinct overview of the major point of the paper Junjun working here ke du ke du ke du ke duResultsThis section is only included in papers that rely on primary research. This section catalogues the results of the experiment. The results should be presented in a clear and unbiased way. Most results sections will contain links and citations, e.g., and equations, e.g. \(e^{i\pi}+1=0\).ConclusionThe conclusion should reinforce the major claims or interpretation in a way that is not mere summary. The writer should try to indicate the significance of the major claim/interpretation beyond the scope of the paper but within the parameters of the field. The writer might also present complications the study illustrates or suggest further research the study indicates is necessary.

MIXTURE OF GAUSSIANS For practice, we’ll first derive the EM algorithm for the Mixture of Gaussians (MoG) model. Natural Parameterization The typical Gaussian distribution p(x) = {}e^{-{2\sigma^2}} can be rewritten in terms of its natural exponential family form p(x) = {}e^{{\sigma^2}x-{2\sigma^2}x^2−\log\sigma−{2\sigma^2}} ={}e^{\alpha x+\beta x^2+{2}\log(-2\beta)+{4\beta}} where $\alpha={\sigma^2}$ and $\beta=-{2\sigma^2}$ and inversely $\mu=-{2\beta}$ and $\sigma={2\beta}}$.

In this document, we will describe alternative versions of SAILnet which address the convergence issues present in the original. The first section [descend] will briefly sketch the sparse approximation equations obtained when the membrane potentials in SAILnet are interpreted as continuous coefficients in our sparse coding model. In section [spike], we will show that a spiking version of our Rate-based Sparse and Independent Local network is guaranteed to descend the objective function .

VECTOR BUNDLES Basic Definitions

CDS&E: REAL-TIME, COMMENSAL FAST RADIO TRANSIENT SURVEYS WITH THE VERY LARGE ARRAY ** to do: systematic references to co-observing resources and commensal VLASS ** _:_ We propose a set of enhancements to the Jansky Very Large Array (VLA) to enable 24/7 surveys for fast radio transients. Large, single-dish radio telescopes have dedicated thousands of hours to surveys for millisecond-scale transients with the aim of capturing rare classes of cosmological transient, understanding the lifecycle of neutron stars, and measuring otherwise inaccessible properties of interstellar and intergalactic material. This field has been revitalized in the past decade with the discovery of new classes of transient. As the most sensitive radio interferometer on earth, the VLA will revolutionize this field with its ability to form sensitive images with unmatched spatial resolution. The core of the proposed system is a 32-node, GPU-accelerated compute cluster that will search images generated on timescales from 1 ms to 1 minute. Real-time processing will allow triggered recording of the parallel data stream for later analysis and the rapid announcement of candidates for follow-up observing. By integrating with a high-speed, duplicate data stream of the VLA, this system will turn each observation into a fast transient survey, ultimately encompassing thousands of hours per year. _:_ Interferometric imaging will do pioneering science with a mysterious new class of radio transients known as “fast radio bursts”. These millisecond transients have inferred distances that imply a cosmological origin and extreme luminosities. Such an event would open a new window on the intergalactic medium and cosmology. Only an interferometer can uniquely identify counterparts (e.g., a host galaxy or gamma-ray burst) well enough to constrain their nature and enable their use as cosmic probes. The proposed system will provide the first arcsecond localization of a burst and will detect more than 12 bursts over the course of the program. Similarly, the interferometric discovery and localization of other classes of millisecond transient will address topics ranging from the missing baryon problem to (sub)stellar magnetism to the search for exotic binary pulsar systems. Time-domain astronomy has been identified as a discovery frontier in the recent Decadal Review of Astronomy and Astrophysics. Real-time, commensal analysis creates discovery potential by searching an otherwise inaccessible data stream. Developing this system at the VLA will produce multiplicative improvement to scientific productivity for this already powerful telescope. _:_ The completed system will autonomously detect radio transients and drive follow-up observing across the electromagnetic spectrum. Co-observing with other observatories, such as the Long Wavelength Array and Skynet, opens novel science and public outreach opportunities. Additional computing power and flexible software at the VLA site will open new observing models. The data analysis software is open source, which allows any astronomer to reproduce VLA detections or integrate the software into other interferometric fast transient surveys. Consider the excitement of seeing a shooting star: a dynamic flash in what seems a static sky. We aim for our transient detection system to inspire similar recognition of the evolving and dynamic sky at timescales faster than the blink of an eye. Alerts will be announced for all new discoveries and will be visualized with movies, images, and spectra to engage the public at NRAO sites and via the web. Opportunities for student training will be available on topics such as transient astrophysics, interferometric algorithms, heterogeneous/high-performance computing, and front-end web development. These topics, and the data-intensive nature of this project, have increasing relevance for academic, commercial, and national security applications.

A substantial amount of research on the security of cyber-physical systems assumes that the physical system model is available to the adversary. In this paper, we argue that such an assumption can be relaxed, given that the adversary might still be able to identify the system model by observing the control input and sensory data from the system. In such a setup, the attack with the goal of identifying the system model using the knowledge of input-output data can be categorized as a Known-Plaintext Attack (KPA) in the information security literature. We first prove a necessary condition and a sufficient condition, under which the adversary can successfully identify the transfer function of the physical system. We then provide a low-rank controller design which renders the system unidentifiable to the adversary, while trading off the LQG performance.

[idea] Surveillance Transactions Lisa goes to a cafe and gets a coffee. She gets a receipt back. On the receipt is a record not only of the financial transaction of exchanging money for coffee, but also the additional "information transactions" that are taking place - Ethnicity: white (this is really race but the label is intentionally off) - Gender: female - Age: 20-30 - Heart rate: 70-80 bpm - Mood: 70% - Purchase: medium coffee (prediction confidence: 50%) - You might like: Chocolate Croissant (recommendation confidence: 75%) - Informatics Value: $0.0001 - Have a nice day! [idea] Emotionally Aware Desk Lamp An office manager has a nice lamp. It sits off to the side of his office, sort of halfway between where he would sit behind his desk and someone would sit in front of his desk to talk with him. It glows in different colors based on the mood valence of the people in the room. It uses the heart rate and GSR of the people in the room to do this, because employees are required to wear Empatica wristbands. The manager thinks the office lamp helps create a more relaxing atmosphere for his conversations with those he manages. He keeps an eye on how it changes color to gauge whether he or the other person is getting tense. The Empatica data of the individuals, and the lamp's averaged data, is collected by the company and used as part of the manager's annual performance report. Unfortunately for this manager, the lamp has reported that there was not enough Focused time in his office, a little too much Relaxed time, and a little too much Tense time. The manager tries to explain that he usually has focused group work meetings in another larger room, and that his office is mostly for personal check ins and mediating employee relations. Unfortunately there is not a lamp in the meeting room, because it would be too complicated for the lamp to take in a variable number of Empatica wristbands' data. dominant metaphors or values: - optimizing for a healthy lifestyle is good - optimizing for productivity is good - the individual should optimize their own life - responsibility for action is on the individual, and the apps / algorithms they employ for help along the way - our body is equal to the sum of its individual components as measurable by technology (organs, data streams, etc) - if you can't measure it with technology, then it isn't real - sharing in an anonymized form is safe - algorithms as neutral / free of human bias - data as neutral / free of human bias (when actually it is created by designers as mentioned above) - Also, the data is something that already "exists" out there, independent of observation (versus something that's being constructed or co-constructed by the observer) - everyday people as consumers of biosensing devices and simultaneously producers of data

THIS IS A PLANNING SPACE FOR THE VLASS MSIP. EDIT SECTIONS BELOW. BE SURE TO “SAVE AND CLOSE” A SECTION ONCE COMPLETE. SECTION 2: DEFINE DATA PRODUCTS (MAPS AND UV DATA) SECTION 3: DEFINE DATA PRODUCTS (CATALOGS) SECTION 4: TITLE SUGGESTIONS

Here, I wish to motivate bilinear system identification techniques for 3 order spectroscopy. The von Neumann equation describes time evolution of a density matrix $\rho = \sum_i p_i $ where $\{\}$ spans the Hilbert space: \[ {t} = -{\hbar}[H(t),\rho(t)]\] Integrating: \[ \rho(t) = \rho(0) + {\hbar}^{t}{dt_1[H(t_1),\rho(t_1)]}\] One can solve by repeatedly inserting the above equation into itself: \[ \rho(t) = \rho(0) + {\hbar}^{t}{dt_1[H(t_1),\rho(0)] + \left({\hbar}\right)^2 ^{t}{dt_1 ^{t_1}{dt_2[H(t_1),[H(t_2),\rho(t_2)]]}}}\] And so on: \[ \rho(t) = \rho(0) + ^{\infty}{\left({\hbar}\right)^n ^{t}{dt_1 ^{t_1}{dt_2 ... ^{t_{n-1}}{dt_n [H(t_1),[H(t_2),...[H(t_n),\rho(t_n)]...]]}}}}\] This series is traditionally defined as \[ \rho(t) = ^{\infty}{\rho_n(t)} = \rho(0) + ^{\infty}{\rho_n(t)} \] where ρ₀(t)=ρ(0) and ρn(t)=∫₀tdt₁...∫₀tn − 1dtn[H(t₁),...[H(tn),ρ(tn)]...]. Re-inspecting the above equation, I find a recursive relationship for the n order perturbation using linearity of the commutator: \[ \rho_n(t) = {\hbar}^{t}{d\tau[H(\tau),(\tau)]} \] By differentiating both sides, I derive an equation of motion for the n order perturbation: \[ {t} = {\hbar}[H(t),(t)] \] In nonlinear spectroscopy, polarization is related to the perturbation of the density matrix as follows (see Mukamel): \[ P_n(t) = \] I wish to use a general form to relate the polarization measurement P₃(t) with n order perturbations of the density matrix. In superoperator form (where the elements of n × n density matrices concatenate to create 1 × n² vectors), let us define $$ as a concatenation of ρn, 0 ≤ n ≤ 3: \[ (t) = \left( {cccc} \rho_0(t) \\ \rho_1(t) \\ \rho_2(t) \\ \rho_3(t) \\ \right)\] The third-order polarization measurement P₃(t) is therefore \[ P_3(t) = \left({c} 0 \\ 0 \\ 0 \\ F \\ \right) \cdot (t)\] such that applying F (in operator form) behaves as follows: $F \cdot = $. The 1 × 4n² vector $(t)$ is governed by the time evolution equation \[ (t)}{t} = \left( {cccc} 0 & 0 & 0 & 0 \\ M(t) & 0 & 0 & 0 \\ 0 & M(t) & 0 & 0 \\ 0 & 0 & M(t) & 0 \\ \right) (t) \] where $(0) = \left( {cccc} \rho(0) \\ 0 \\ 0 \\ 0 \\ \right) $ and applying M(t) (in operator form) behaves as follows: $M(t) \cdot = {\hbar}[H(t),\cdot]$. This is a general form to describe polarization measurement P₃(t) and perturbations of the density matrix.

Data structures are the foundation upon which computational tools are built. For example, the simple pointer-to-memory approach, established by languages such as Fortran and C, acts as a _de facto_ standard by which different packages and libraries can interoperate with a single shared array of numerical data in memory. While this simple abstraction for n-dimensional arrays has served us well in the past, there is a clear need for data structures that have richer semantics and make it easy to express and manipulate common forms of (semi-)structured data. This need is highlighted by the popularity of R’s data frames and Python libraries, such as bcolz (column storage), pandas (indexed data frames), and X-ray (n-dimensional indexed arrays). This paper aims to present the state of the art in data structures, across programming languages and implementation details, that are foundational in data science, scientific computing, and statistical applications. It will review current data representation semantics implemented by various libraries, packages, and languages, with an explicit emphasis on interoperability across languages and process boundaries.

The core rotation rates of massive stars have a substantial impact on the nature of core collapse supernovae and their compact remnants. We demonstrate that internal gravity waves (IGW), excited via envelope convection during a red supergiant phase or during vigorous late time burning phases, can have a significant impact on the rotation rate of the pre-SN core. In typical (10 M⊙ ≲ M ≲ 20 M⊙) supernova progenitors, IGW may substantially spin down the core, leading to iron core rotation periods $P_{\rm min,Fe} \gtrsim 50 \, {\rm s}$. Angular momentum (AM) conservation during the supernova would entail minimum NS rotation periods of $P_{\rm min,NS} \gtrsim 3 \, {\rm ms}$. In most cases, the combined effects of magnetic torques and IGW AM transport likely lead to substantially longer rotation periods. However, the stochastic influx of AM delivered by IGW during shell burning phases inevitably spin up a slowly rotating stellar core, leading to a maximum possible core rotation period. We estimate maximum iron core rotation periods of $P_{\rm max,Fe} \lesssim 10^4 \, {\rm s}$ in typical core collapse supernova progenitors, and a corresponding spin period of $P_{\rm max, NS} \lesssim 400 \, {\rm ms}$ for newborn neutron stars. This is comparable to the typical birth spin periods of most radio pulsars. Stochastic spin-up via IGW during shell O/Si burning may thus determine the initial rotation rate of most neutron stars. For a given progenitor, this theory predicts a Maxwellian distribution in pre-collapse core rotation frequency that is uncorrelated with the spin of the overlying envelope.

INTRODUCTION - KEY SCIENCE GOALS, CONTEXT, AND THE FAST/SLOW TRANSIENT SPLIT The paper will present an overview of the science, techniques, and state-of-the-art of surveys for radio transients. The paper is aimed to non-experts such as early graduate students who are interested in working in the field, but will also provide detailed information for researchers currently working in the field. Progress in the field is rapid so there will be a heavy emphasis on long-term science goals and technqiues. I will discuss important developing topics such as fast radio bursts, where there is still considerable uncertainty about the significance of current discoveries. The science and techniques of radio transient surveys are divided into domains: fast and slow. The dividing line is a characteristic time scale of 1 second. On short time scales, coherent emission processes such as the pulsar mechanism dominate. On longer time scales, incoherent synchrotron processes dominate. Technically, slow transient searches are in the domain of interferometric imaging. Fast transient searches have been traditionally the domain of high bandwidth single dish timing. Interferometric techniques, however, are becoming more important for fast transient searches. The next generation of large telescopes are primarily large-N interferometers. As these new telescopes are commissioned, interferometric techniques must be expoited in order for fast transient searches to advance scientifically. The science of radio transients has primarily been driven by follow-up of optical and high energy events such as gamma-ray bursts and supernovae. Surveys have the opportunity to discover new classes of transient that are not known or predicted by multi-wavelength information. Serendipitous discovery has demonstrated that radio transient surveys can be critical for discovery of dust-obscured objects and coherent emitters that would not have been otherwise discovered. There is the potential for new radio transient surveys to flip the dominant paradigm in which radio discovery leads to optical and high energy follow-up. The paper is timely because of the launch of major surveys with the Very Large Array and LOFAR and the planned launch of surveys with ASKAP and MeerKAT. Pre-cursor surveys with the VLA, the Allen Telescope Array, Parkes, Arecibo, and the GBT provide an important foundation for planning. The coming of Advanced LIGO GW interferometer results at the end of the decade will heighten interest in disovery of radio transient counterparts to GW events.

The core rotation rates of massive stars have a substantial impact on the nature of core collapse supernovae and their compact remnants. We demonstrate that internal gravity waves (IGW), excited via envelope convection during a red supergiant phase or during vigorous late time burning phases, can have a significant impact on the rotation rate of the pre-SN core. In typical (10 M⊙ ≲ M ≲ 20 M⊙) supernova progenitors, IGW may substantially spin down the core, leading to iron core rotation periods $(P_{\rm min,Fe} \gtrsim 50 \, {\rm s})$. Angular momentum (AM) conservation during the supernova would entail minimum NS rotation periods of $P_{\rm min,NS} \gtrsim 3 \, {\rm ms}$. In most cases, the combined effects of magnetic torques and IGW AM transport likely lead to substantially longer rotation periods. However, stochastic influxes of AM delivered by IGW during shell burning phases also entail a maximum core rotation period. We estimate maximum iron core rotation periods of $P_{\rm max,Fe} \lesssim 10^4 \, {\rm s}$ in typical core collapse supernova progenitors, and a corresponding spin period of $P_{\rm max, NS} \lesssim 400 \, {\rm ms}$ for newborn neutron stars. This is comparable to the typical birth spin periods of most radio pulsars. Stochastic spin-up via IGW during shell O/Si burning may thus determine the initial rotation rate of most ordinary pulsars. For a given progenitor, this theory predicts a Maxwellian distribution in pre-collapse core rotation frequency that is uncorrelated with the spin of the overlying envelope.

OVERVIEW This working document details the Technical Implementation Plan (TIP) for the VLA Sky Survey (VLASS). The main Survey Science proposal “The Jansky Very Large Array Sky Survey (VLASS)” contains the science justification and overall description of the survey. This supplementary document describes in more detail the technical issues, project plan, and risks associated with the proposed VLASS. _Version Note:_ current draft reflects Pilot Survey implementation and updates for the PDR Version Milestones: _2016-08-25_ — draft for the Preliminary Design Review in Sep 2016. _2015-10-02_ — draft reflects the revisions to the survey following the Community Review in March 2015. _2015-02-02_ — version submitted to Community Review

INTRODUCTION The “fast radio burst” (FRB) is a new class of transient found in a variety of single-dish pulsar surveys . FRBs are identified by their large dispersion measure (DM), which has been observed as high as 1100 pc cm−3, an order of magnitude larger than expected from the Galaxy. The simplest explanation for this large DM is that the bursts are dispersed by the intergalactic medium (IGM), implying that they originate at distances up to z∼1. If FRBs are cosmological, then they could be used to probe the intergalactic medium and study processes for their formation \citep[e.g., double neutron star mergers][]{2013PASJ...65L..12T}. However, terrestrial phenomena known as perytons have been discovered at the same telescopes finding FRBs . Perytons are impulsive radio transients with a width of tens of ms and an apparent DM of a few hundred, partially overlapping with characteristics expected of extragalactic radio transients. suggest that perytons and FRBs are the same, terrestrial process seen in different optical regimes of the telescopes. It will be critical to distinguish these populations to be certain that FRBs are are astrophyiscal. One way to understand their nature is to build statistical tests... Euclidean distribution... Rate constraint for future observing campaigns... We are in the midst of a large survey with the Karl G. Jansky Very Large Array (VLA) to detect an FRB \citep[results in][]{law2014a}. The nondetection in that survey inspired us to reanalyze published rates in an attempt to make a reliable prediction for FRB rates for any given survey. Here, we present our estimate of the apparent flux distribution of FRBs to determine if they are consistent with an astrophysical population. We then use a Bayesian technique to estimate the FRB rate for a given telescope flux limit.

stars: formation — stars: Population III — cosmology: theory — early Universe — dark ages, first stars

SUMMARY We report on the state of observing for the VLA FRB project, also known as 13B-409 and 14A-425. We detected no FRBs in the first 76 hours observed under an approved DDT proposal (13B-409). Comparing our rate constraint to published rates revealed inconsistencies in published rates that led to an overestimate of the chance for a VLA detection. We discuss an improved rate estimate and find that completing the 147-hour campaign under program 14A-425 will give us a 50% chance at detecting an FRB. The completed VLA observations are the first interferometric search for FRBs and have already highlighted the value of using an interferometer to define a robust FRB rate limit. Ensuring that 14A-425 is observed to completion will significantly improve our chances of making the first interferometric detection of an FRB; an extremely exciting scientific result. CURRENT STATUS Observations took place between late September 2013 and mid January 2014 (see Table [fields]). The array was in CnB configuration for the first 10 hours observed, was being reconfigured during the next 10 hours of observing, and was in B configuration for the final 56 hours observed. We observed for a total of 76 hours and were on our target fields for 63.3 hours for an observing efficiency of 83%. ----------- ------------ ------------- ------- Name RA Dec Time (J2000) (J2000) (hrs) RA02 2:27:52.7 +9:13:24.3 2 CDF-South 3:32:28.0 –27:48:30.0 4 RA05 5:04:37.0 –30:50:0.1 16 COSMOS 10:00:28.6 +2:12:21.0 10 RA12 12:00:7.2 +5:53:12.0 4 FRB120127 23:15:00 –18:25:00 40 ----------- ------------ ------------- ------- : Fields for September 2013 to January 2014 FRB Campaign All 63.3 hours of time on extragalactic fields has been searched for transients with dispersion measures from 0 to 3000 pc cm−3 at a timescale of 5 ms. Figure [snrhist] shows the typical SNR histogram of candidates greater than 6.5σ, which are saved for analysis. Nearly all candidates are consistent with thermal noise. Eight candidates deviated slightly from the thermal noise distribution and were inspected in detail. All of these candidates were found to be affected by RFI or were highly sensitive to flagging or imaging parameters. Our analysis shows that we can exclude the presence of astrophysical transients on timescales of 5 milliseconds and below. We measured data quality at regular intervals throughout the search and found that roughly 1% of images had noise that was more than twice the median image noise. Our flux-calibrated observations have a median image noise of 12–14 mJy, as expected for 5-ms, L-band images made with data from 26 good antennas and 230 MHz of bandwidth. To include variance in the noise measurements, we define a 96% completeness for a 1σ image sensitivity of 15 mJy or an 8σ flux limit of 120 mJy. Observations of pulsar B0355+54 at a range of offset positions shows that imaging sensitivity scales as expected for the VLA primary beam gain pattern. This end-to-end test also confirms that our transient search pipeline works as expeted. Figure [rate_pub] summarizes the published FRB event rates and the VLA rate limit to FRBs shorter than our integration time of 5 ms. In constructing this figure, we discovered that the sensitivity of published surveys are defined inconsistently. calculate the mean beam gain within the FWHM. Burke-Spolaor & Bannister (2014, submitted; hereafter “BSB14”) use half the main beam gain. use the measured fluence of their detection to define a fluence limit. Finally, don’t report a fluence limit at all, but instead measure the mean fluence of all detections. For this figure, we use the mean primary beam gain, as in , although this clearly overestimates the sensitivity at the half-power point, as demonstrated in our pulsar tests.