text:
Deadliest Catch: The Game Has Left Early Access, Heading to Consoles Later This Year
Deadliest Catch: The Game
Deadliest Catch: The Game, a simulator of a king crab fisherman based on the popular Discovery Channel series, has left Early Access. As announced by Ultimate Games S.A., the game will also be released on PlayStation 4, Xbox One and Nintendo Switch. Console versions of Deadliest Catch: The Game are expected to appear in Q4 2020 or Q1 2021.
The simulator was created by Moonlit S.A., a studio located in Cracow, Poland. The game debuted on Steam Early Access on November 14, 2019, and the final release has been set to April 14, 2020. The game is being published on PC by Ultimate Games S.A., which will also be responsible for console conversions.
Deadliest Catch: The Game is a realistic 3D simulator created in cooperation with the Discovery Channel and Discovery Game Studios. It allows the players to catch king crabs in the Bering Sea and manage a special fishing boat (the so-called "crabber"). The creators have paid particular attention to details, and the gameplay itself combines realism and approachability.
"While in Early Access, Deadliest Catch: The Game was well received by the players. As of today, the percentage of positive reviews has reached almost 70%. In recent months, the game has been improved upon and expanded with new features, in accordance with the previous plan and player feedback. Thanks to this, the game recreates the conditions known from the popular Discovery channel even more faithfully" – explains Mateusz Zawadzki, CEO at Ultimate Games S.A.
The king crab fisherman simulator gives the players a lot of different possibilities. For example, they will be preparing the expedition and striving to stick to the chosen course. The developers from Moonlit S.A. have also created, among others, realistic water physics and dynamic weather systems.
Deadliest Catch: The Game – main features:
Advanced king crab fishing methods;
Realistic gameplay;
Extensive ship and crew management options;
Dynamic weather system;
Advanced water physics;
Ship expansion and improvement possibilities;
Game based on the popular Discovery Channel series.
The demo for Deadliest Catch: The Game is available on Steam.
Showing comments 1-3 of 3 comments
wcsutto 04-19-2020 10:39:35 AM (EDT)
Um, Operations Sports?
Cardot 04-21-2020 01:45:14 PM (EDT)
I was pretty good at this back in the day.
dickey1331 05-03-2020 04:06:46 AM (EDT)
Do I get to be saved by myself in the game?
Related Topics:Deadliest Catch: The Game, Deadliest Catch: The Game demo, Deadliest Catch: The Game screenshots, Deadliest Catch: The Game trailer
More in Deadliest Catch: The Game


Supplemental Health Care is a nationally recognized healthcare staffing provider partnering with a hospital in beautiful Nantucket, MA to provide a Travel Labor and Delivery RN.
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text:
Safety and feasibility of ultrasound-triggered targeted drug delivery of doxorubicin from thermosensitive liposomes in liver tumours (TARDOX): a single-centre, open-label, phase 1 trial.
Lyon PC., Gray MD., Mannaris C., Folkes LK., Stratford M., Campo L., Chung DYF., Scott S., Anderson M., Goldin R., Carlisle R., Wu F., Middleton MR., Gleeson FV., Coussios CC.
BACKGROUND:Previous preclinical research has shown that extracorporeal devices can be used to enhance the delivery and distribution of systemically administered anticancer drugs, resulting in increased intratumoural concentrations. We aimed to assess the safety and feasibility of targeted release and enhanced delivery of doxorubicin to solid tumours from thermosensitive liposomes triggered by mild hyperthermia, induced non-invasively by focused ultrasound. METHODS:We did an open-label, single-centre, phase 1 trial in a single UK hospital. Adult patients (aged ≥18 years) with unresectable and non-ablatable primary or secondary liver tumours of any histological subtype were considered for the study. Patients received a single intravenous infusion (50 mg/m2) of lyso-thermosensitive liposomal doxorubicin (LTLD), followed by extracorporeal focused ultrasound exposure of a single target liver tumour. The trial had two parts: in part I, patients had a real-time thermometry device implanted intratumourally, whereas patients in part II proceeded without thermometry and we used a patient-specific model to predict optimal exposure parameters. We assessed tumour biopsies obtained before and after focused ultrasound exposure for doxorubicin concentration and distribution. The primary endpoint was at least a doubling of total intratumoural doxorubicin concentration in at least half of the patients treated, on an intention-to-treat basis. This study is registered with ClinicalTrials.gov, number NCT02181075, and is now closed to recruitment. FINDINGS:Between March 13, 2015, and March 27, 2017, ten patients were enrolled in the study (six patients in part I and four in part II), and received a dose of LTLD followed by focused ultrasound exposure. The treatment resulted in an average increase of 3·7 times in intratumoural biopsy doxorubicin concentrations, from an estimate of 2·34 μg/g (SD 0·93) immediately after drug infusion to 8·56 μg/g (5·69) after focused ultrasound. Increases of two to ten times were observed in seven (70%) of ten patients, satisfying the primary endpoint. Serious adverse events registered were expected grade 4 transient neutropenia in five patients and prolonged hospital stay due to unexpected grade 1 confusion in one patient. Grade 3-4 adverse events recorded were neutropenia (grade 3 in one patient and grade 4 in five patients), and grade 3 anaemia in one patient. No treatment-related deaths occurred. INTERPRETATION:The combined treatment of LTLD and non-invasive focused ultrasound hyperthermia in this study seemed to be clinically feasible, safe, and able to enhance intratumoural drug delivery, providing targeted chemo-ablative response in human liver tumours that were refractory to standard chemotherapy. FUNDING:Oxford Biomedical Research Centre, National Institute for Health Research.
The Lancet. Oncology
Nuffield Department of Surgical Sciences, John Radcliffe Hospital, Oxford University Hospitals NHS Foundation Trust, Oxford, UK; Department of Radiology, Churchill Hospital, Oxford University Hospitals NHS Foundation Trust, Oxford, UK; Institute of Biomedical Engineering, University of Oxford, Oxford, UK.

redpajama_set_name: RedPajamaCommonCrawl


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People around the world have been reporting hearing hums, musical blasts, horns, or other trumpet-like sounds from the sky or even from the earth itself. Reports from the United States, Canada, Costa Rica, Russia, Australia, the Czech Republic, and other places describe a unique sound with groaning qualities interspersed with metallic, vibrating, musical-like qualities. Some report hearing sorts of voices that can't be understood.
Are these sounds man-made, natural, or supernatural? A few theories have surfaced.
First, some believe the sounds are caused by solar plasma and the magnetic field of the earth interacting, or the movement of tectonic plates. Some say it is the sound of the earth's north magnetic pole shifting. If these are accurate sources of the sounds, why weren't they reported before March 2011?
Maybe these sounds are from aliens visiting the earth. Some say these sounds are pranks. Videos posted online broadcasting the sounds can be easily reproduced complete with astounded onlookers. Others dismiss the supernatural possibilities by tracing the sounds to industry or military sources, including the HAARP and Project Blue Beam theories. Some say a government or group of nations is altering the weather, using micro-waves, or trying to create similar conditions to the return of Jesus.
But, could it be these sky trumpets have a supernatural or spiritual origin? While some believe these sounds are God's way of warning us the end days are coming, others believe Satan is generating them to scare us.
Heavenly trumpets do exist and God has employed them in the past and has designs to use them again. In Exodus 19:16, a loud trumpet blast accompanied God's presence on Mt. Sinai when He gave the Law. This sound grew in intensity (verse 19).
In the future, the rapture of Jesus' followers will be announced by a trumpet sound (1 Corinthians 15:52). In Matthew 24:31, Jesus talked about His second coming this way: "And he will send out his angels with a loud trumpet call, and they will gather his elect from the four winds, from one end of heaven to the other."
John describes seven angels who usher in judgments on the earth during the end times tribulation with seven trumpets (Revelation 8—9). The recent sounds cannot be these trumpet sounds because the tribulation has not begun. And, because the rapture hasn't occurred, the sky trumpets heard in the last few years are not the "last trumpet" mentioned in 1 Corinthians 15:52.
In conclusion, the likeliest explanation for these sky trumpets, biblically speaking, is that they are man-made or naturally occurring. We do know that the last times described in the Bible will be accompanied by increased wickedness and more and more false teaching (1 Timothy 4:1; 2 Timothy 4:3; Jude 1:18). These will increase after the rapture (2 Thessalonians 2:9–11).
People concerned about sky trumpets should be more concerned with the state of their souls—their relationship with Jesus.


Background & Aim: Individuals' perception of organizational justice is very important. The aim of this study was to identify the relationship between organizational justice and psychological empowerment of nurses working in hospitals affiliated to Shahid Beheshti University of Medical Sciences.
Material & Methods: It was a descriptive- correlational study. The sample consisted of 155 nurses working in hospitals affiliated to Shahid Beheshti University of Medical Sciences who were recruited by random stratified sampling during 2012. Data was collected by Niehooff and Moorman's Organizational Justice questionnaire and Spreitzer's Psychological Empowerment instrument and analyzed by descriptive statistics, Pearson correlation coefficient and multiple regression using SPSS-PC (v. 16).
Results: A significant positive correlation was found between organizational justice and nurses' psychological empowerment (p= 0.005). Also the results of multiple regression showed that interactional justice can explain %53 of the variance of Psychological empowerment of nurses.
Conclusion: Regarding the significant relationship between organizational justice and nurses' psychological empowerment, managers' attention to organizational justice of healthcare system to improve the nurses' psychological empowerment is suggested.
6. Folger RG, Cropanzano R. Organizational justice and human resource management: sage publications; 1998.
11. Abdollahi B. [Psychological Empowerment: Dimensions and Validation on the Structural Equation Model]. Quarterly Journal of Research and Planning in Higher Education. 2005;11(1):37-63.
14. Ebrahimi H, Hosseinzadeh R, Zaghari Tefreshi M, Hosseinzadeh S, Asghari Jafarabadi M. [Clinical competency and psychological empowerment of nurses and their correlation with demographic characteristics]. Journal of Health Promotion Management. 2013;2(4):30-8.
15. Laschinger HKS, Finegan J. Using empowerment to build trust and respect in the workplace: A strategy for addressing the nursing shortage. Nursing Economics. 2005;23(1):6. 13.
19. Yaghmaei F. [Content validity and its estimation]. J Med Educ. 2003; 3(1) :25-7.
23. Eskandari F, Pazargadi M, Zagheri Tafreshi M, Rabie Siahkali S, Shoghli AR. [Relationship between Psychological Empowerment with Affective Commitment among Nurses in Zanjan, 2010]. Preventive Care in Nursing & Midwifery Journal. 2014;3(2):47-60.


Abstract: This guide provides an overview of the problem of juvenile runaways and its risk factors. The guide also identifies a series of questions to help you analyze your local juvenile runaways problem. Finally, it reviews responses to the problem and what is known about them from evaluative research and police practice.


text:
Q: Add Jar to standalone pyspark I'm launching a pyspark program:
$ export SPARK_HOME=
$ export PYTHONPATH=$SPARK_HOME/python:$SPARK_HOME/python/lib/py4j-0.9-src.zip
$ python

And the py code:
from pyspark import SparkContext, SparkConf

SparkConf().setAppName("Example").setMaster("local[2]")
sc = SparkContext(conf=conf)

How do I add jar dependencies such as the Databricks csv jar? Using the command line, I can add the package like this:
$ pyspark/spark-submit --packages com.databricks:spark-csv_2.10:1.3.0

But I'm not using any of these. The program is part of a larger workflow that is not using spark-submit I should be able to run my ./foo.py program and it should just work.

*

*I know you can set the spark properties for extraClassPath but you have to copy JAR files to each node?

*Tried conf.set("spark.jars", "jar1,jar2") that didn't work too with a py4j CNF exception

A: I encountered a similar issue for a different jar ("MongoDB Connector for Spark", mongo-spark-connector), but the big caveat was that I installed Spark via pyspark in conda (conda install pyspark). Therefore, all the assistance for Spark-specific answers weren't exactly helpful. For those of you installing with conda, here is the process that I cobbled together:
1) Find where your pyspark/jars are located. Mine were in this path: ~/anaconda2/pkgs/pyspark-2.3.0-py27_0/lib/python2.7/site-packages/pyspark/jars.
2) Download the jar file into the path found in step 1, from this location.
3) Now you should be able to run something like this (code taken from MongoDB official tutorial, using Briford Wylie's answer above):
from pyspark.sql import SparkSession

my_spark = SparkSession \
    .builder \
    .appName("myApp") \
    .config("spark.mongodb.input.uri", "mongodb://127.0.0.1:27017/spark.test_pyspark_mbd_conn") \
    .config("spark.mongodb.output.uri", "mongodb://127.0.0.1:27017/spark.test_pyspark_mbd_conn") \
    .config('spark.jars.packages', 'org.mongodb.spark:mongo-spark-connector_2.11:2.2.2') \
    .getOrCreate()

Disclaimers:
1) I don't know if this answer is the right place/SO question to put this; please advise of a better place and I will move it.
2) If you think I have errored or have improvements to the process above, please comment and I will revise.

A: 2021-01-19 Updated
There are many approaches here (setting ENV vars, adding to $SPARK_HOME/conf/spark-defaults.conf, etc...) other answers already cover these. I wanted to add an answer for those specifically wanting to do this from within a Python Script or Jupyter Notebook.
When you create the Spark session you can add a .config() that pulls in the specific Jar file (in my case I wanted the Kafka package loaded):
spark = SparkSession.builder.appName('my_awesome')\
    .config('spark.jars.packages', 'org.apache.spark:spark-sql-kafka-0-10_2.12:3.0.1')\
    .getOrCreate()

Using this line of code I didn't need to do anything else (no ENVs or conf file changes).

*

*Note 1: The JAR file will dynamically download, you don't need to manually download it.

*Note 2: Make sure the versions match what you want, so in the example above my Spark version is 3.0.1 so I have :3.0.1 at the end.

A: Finally found the answer after a multiple tries. The answer is specific to using spark-csv jar. Create a folder in you hard drive say D:\Spark\spark_jars. Place the following jars there:

*

*spark-csv_2.10-1.4.0.jar (this is the version I am using)

*commons-csv-1.1.jar

*univocity-parsers-1.5.1.jar

2 and 3 are dependencies required by spark-csv, hence those two files need to be downloaded too. Go to your conf directory where you have downloaded Spark. In the spark-defaults.conf file add the line:
spark.driver.extraClassPath D:/Spark/spark_jars/*
The asterisk should include all the jars. Now run Python, create SparkContext, SQLContext as you normally would. Now you should be able to use spark-csv as
sqlContext.read.format('com.databricks.spark.csv').\
options(header='true', inferschema='true').\
load('foobar.csv')

A: Any dependencies can be passed using spark.jars.packages (setting spark.jars should work as well) property in the $SPARK_HOME/conf/spark-defaults.conf. It should be a comma separated list of coordinates.
And packages or classpath properties have to be set before JVM is started and this happens during SparkConf initialization. It means that SparkConf.set method cannot be used here.
Alternative approach is to set PYSPARK_SUBMIT_ARGS environment variable before SparkConf object is initialized:
import os
from pyspark import SparkConf

SUBMIT_ARGS = "--packages com.databricks:spark-csv_2.11:1.2.0 pyspark-shell"
os.environ["PYSPARK_SUBMIT_ARGS"] = SUBMIT_ARGS

conf = SparkConf()
sc = SparkContext(conf=conf)

A: import os
import sys
spark_home = os.environ.get('SPARK_HOME', None)
sys.path.insert(0, spark_home + "/python")
sys.path.insert(0, os.path.join(spark_home, 'python/lib/py4j-0.10.4-src.zip'))

Here it comes....
sys.path.insert(0, <PATH TO YOUR JAR>)

Then...
import pyspark
import numpy as np

from pyspark import SparkContext

sc = SparkContext("local[1]")
.
.
.

A: From working with PySpark, PostgreSQL, and Apache Sedona, I learned to solve this with 2 methods.

Method 1: Download the JAR file and add to spark.jars
In order to use PostgreSQL on Spark, I needed to add the JDBC driver (JAR file) to PySpark.
First, I created a jars directory in the same level as my program and store the postgresql-42.5.0.jar file there.
Then, I simply add this config to SparkSession with:
SparkSession.builder.config("spark.jars", "{JAR_FILE_PATH}")
spark = (
    SparkSession.builder
    .config("spark.jars", "jars/postgresql-42.5.0.jar")
    .master("local[*]")
    .appName("Example - Add a JAR file")
    .getOrCreate()
)

Method 2: Use Maven Central coordinate and spark.jars.packages
If your dependency JAR files are available on Maven, you can use this method and not have to maintain any JAR file.
Steps

*

*Find your package on Maven Central Repository Search

*Select the correct package artifact and copy the Maven Central coordinate

*In Python, call SparkSession.builder.config("spark.jars.packages", "{MAVEN_CENTRAL_COORDINATE}").
spark = (
    SparkSession.builder
    .appName('Example - adding many Maven packages')

    .config("spark.serializer", KryoSerializer.getName)
    .config("spark.kryo.registrator", SedonaKryoRegistrator.getName)
    .config("spark.jars.packages",
            "org.postgresql:postgresql:42.5.0,"
            + "org.apache.sedona:sedona-python-adapter-3.0_2.12:1.2.1-incubating,"
            + "org.datasyslab:geotools-wrapper:1.1.0-25.2")

    .getOrCreate()
 )

Pros of using sparks.jars.packages

*

*You can add several packages

*You don't have to manage the fat JAR files

Cons of using sparks.jars.packages
The .config("sparks.jars.packages", ...) accept a single parameter, so in order to add several packages, you need to concatenate the package coordinates using , as the delimiter.
"org.postgresql:postgresql:42.5.0,"
+ "org.apache.sedona:sedona-python-adapter-3.0_2.12:1.2.1-incubating,"
+ "org.datasyslab:geotools-wrapper:1.1.0-25.2"

*** The string will not tolerate next line, spaces, or tabs in your code and it will cause nasty bugs that gives out irrelevant error logs.

redpajama_set_name: RedPajamaStackExchange


The Mantis Mover makes moving large and over-sized loads easy. This is a must have accessory for any party rental business or organization that handles large shipments. It has 34" long forks that makes moving inflatables, folding chairs and other bulky items a snap. The dolly's center forks are 7/8" diameter, 14 3/4" apart, and are made for heavy duty hauling. The 10" solid foam wheels provide you with a piece of mind that you never need to worry about rough or uneven terrain. This dolly's aluminum fenders and an expanded metal back guard protect the load from rubbing on the tires. The Mantis Mover has a strong, rugged design with closed cell foam tires, ball bearing hubs and a powder coated steel frame.
Dimensions: 27" x 39" x 74"


text:
Vinny Gorgeous Basciano sentenced to life in prison plus ten years at Supermax
Vinny 'Gorgeous' Basciano will spend the rest of his life at Colorado's Supermax prison with some of the nation's most notorious criminals.
Bloodthirsty ex-crime boss Vincent Basciano made a startling admission on Wednesday before he was dispatched to rot behind bars in America's toughest federal prison.
"I was done in by the tapes," the murderous mobster said in federal court, referring to damning jailhouse recordings secretly made by ex-Bonanno chief Joseph Massino.
Basciano - spared the death penalty last month by a Brooklyn jury - received a sentence of life plus 10 years from Federal Judge Nicholas Garaufis.
"No punishment is sufficient to right his innumerable wrongs," said Garaufis, who prosecutors say was targeted for murder by Basciano, who is known as "Vinny Gorgeous."
"No words are strong enough to convey the depravity with which he lived his free life."
The 51-year-old gangster is already serving a life sentence for a previous murder. He strode into the courtroom smiling and carrying a carton filled with legal papers.
Asked if he wanted to make a statement about murder victim Randolph Pizzolo, Basciano instead whined about his woes.
"I'm broke, I have no money," he said during a rambling speech, griping that he was denied a fair trial and demanding a new lawyer so he could sue an inmate who snitched on him.
The Basciano jury cited Massino's bloodier past - including a dozen murders - in deciding on a life sentence rather than death for Vinny Gorgeous.
Basciano was convicted of capital murder for ordering a November 2004 mob hit against Bonanno associate Pizzolo. He was previously found guilty in the 2001 murder of Bronx junkie Frank Santoro.
He's headed for the super-maximum security prison in Florence, Colo., where he will join the worst of the worst inmates in Cell Block H.
Basciano's neighbors will include terrorists like World Trade Center bomber Ramzi Yousef and shoe-bomber Richard Reid.
Despite his claimed lack of cash, prosecutors said they intend to collect a $5 million forfeiture order from Basciano's prior trial - and repay the Pizzolo family $21,000 in funeral expenses.
The judge noted that Basciano is proof there is no glory in the Mafia. "Basciano stands here today, proof of its reality - a crumbling facade, beneath which lies a bleak, pathetic and ignorant life," Garaufis said.
http://www.nydailynews.com/news/ny_crime/2011/07/20/2011-07-20_vinny_gorgeous_basciano_sentenced_to_life_in_prison_plus_ten_years_at_supermax_p.html#ixzz1T5C0UwNn
Vinny Gorgeous sentencing: Gangster will kill behind bars if he's not executed, says prosecutor (fivefamiliesnyc.blogspot.com)
"Vinny Gorgeous" wants to take his radio to Super Max (fivefamiliesnyc.blogspot.com)
Vincent "Vinny Gorgeous" Basciano squares off with Brooklyn judge in tense standoff (fivefamiliesnyc.blogspot.com)
Daughter of mob murder victim says Vinny Gorgeous should have been given death penalty (fivefamiliesnyc.blogspot.com)
Vinny Gorgeous faces ugly life in Colorado Supermax prison if he avoids death penalty (fivefamiliesnyc.blogspot.com)
Crime boss 'Vinny Gorgeous' saved my son's life testifies witness (fivefamiliesnyc.blogspot.com)
Let my cousin Vinny live! Family member testifies for mobster Vinny Gorgeous in penalty phase (fivefamiliesnyc.blogspot.com)
I never tried to kill you, murderous mobster Vinny Gorgeous tells judge in secret sitdown (fivefamiliesnyc.blogspot.com)
Mob boss Vincent "Vinny Gorgeous" Basciano dodges death penalty, sentenced to life in prison (fivefamiliesnyc.blogspot.com)
Vinny Gorgeous rips into his lawyer over possible use of the defense (fivefamiliesnyc.blogspot.com)
Bonanno Crime Family / Joseph Massino / Vincent Basciano


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It's officially time for Rita Ora!
In a reveal made moments ago, the 27-year-old unveiled the set's cover (above) and release date – November 23rd.
Beyond confirming that pre-orders will grant fans early ticket access to a European tour, additional tea wasn't poured.
It's safe to assume, though, that the title purposefully draws on Ora's journey up until this point.
Because juxtaposed with her undeniable success and soaring profile is label drama, legal wrangles, and a period of uncertainty over her music career.
Now, come November, Ms. Ora will be rising through the ashes like the 'Phoenix' she is.
We're all sorts of buzzed for her and are keen to hear what she's been cooking up, as well as which tracks will populate the LP.


text:
Capgemini supports Esaote to digitally transform its processes into a Smart Factory model with SAP® solutions
Milan, Paris, March 12, 2018 – Capgemini in Italy has supported Esaote, the world's leading manufacturer of medical diagnostic systems, to undertake a rapid digital transformation based on SAP® solutions, aimed at improving the efficiency of its production processes as well as reducing time-to-market and costs. Departments across the entire company have benefited from the new 'Smart Factory' model.
Esaote has more than 1,200 employees worldwide. With its own production and research units in Italy and The Netherlands, Esaote is recognized as one of the top 10 diagnostic imaging companies in the world. Active in Research and Development, the company has been at the forefront of biomedical systems' innovation for over 30 years. Esaote needed to harmonize the production processes in its plants to gain production efficiencies and optimization in order to reduce costs, through leaner cycles. It also wanted to achieve less production defects to enable scrap and rework cost reductions, and correct plant maintenance strategies to improve overall component traceability.
A transformed technological architecture
To address these challenges Capgemini devised a transformation aimed at harmonizing and simplifying Esaote's technological architecture, through SAP solutions based on the 'LifeSciencesPath'[2] vertical approach, designed in accordance with the sector's best practices. The full implementation of these solutions was achieved in less than 10 months.
"Esaote wanted to digitize its business processes and create efficiencies by adopting a unique and integrated way to manage them. Capgemini helped us to achieve a rapid transformation of our technological and production infrastructure into a Smart Factory model with SAP solutions. With a constantly controlled, performing and abundant IT architecture ensuring service continuity to all users, we can better plan and monitor the production of our probes in a timely manner while reducing the work-in-progress and scrap costs," said Mauro Roncari, CIO at Esaote. "This important step in our IT architecture's modernization process – a pillar for our company – provides a sturdy and reliable basis to manage our business globally."
Real-time connection enhancing production
Thanks to real-time integration with machines and the speed of data processing as well as the quality control framework, it is now possible to capture diagnostic images and compare them with target scans, which verify the correct set up of probes. With the real-time connection removing the need for physical interaction between operator and machine, the operator can focus on collecting and analyzing data and recording measurements, all supported by automated management of the non-compliance issues.
Performance is now monitored in real-time with KPIs and analytics. The solution is highly scalable as it defines processes enabling the production management to then map machines, workstations, skills, operations' lines and sequences that need to be performed.
Gerardo Ciccone, Head of Manufacturing & Life Science at Capgemini in Italy, said: "We brought together our expertise in digital manufacturing with SAP solutions to support Esaote in achieving its goal of transforming its technological infrastructure with a Global 'Industry 4.0' platform. It now optimizes and manages a fully integrated and scalable production process within a comprehensive network of suppliers, customers, and post-sales services. We worked closely with the Esaote teams, in a very collaborative way, to identify the best process solutions for the systems."
Capgemini integrated Esaote infrastructure with SAP solutions[3] , leveraging the "Fast Digital 4 Discrete Industries" (FD4DI) offering, a Capgemini and SAP joint initiative to help clients in discrete manufacturing industries manage their digital transformation, as they seek to adopt innovative concepts driven by 'Industry 4.0', the industrial Internet of Things (IoT), Cloud, Big Data, and Smart Automation. FD4DI provided the Digital Transformation framework, centered on digital experience to achieve excellence and agile processes, with the coverage of end to end processes from Sales to Operations.
Illustrative high-resolution images are available on request
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A global leader in consulting, technology services and digital transformation, Capgemini is at the forefront of innovation to address the entire breadth of clients' opportunities in the evolving world of cloud, digital and platforms. Building on its strong 50-year heritage and deep industry-specific expertise, Capgemini enables organizations to realize their business ambitions through an array of services from strategy to operations. Capgemini is driven by the conviction that the business value of technology comes from and through people. It is a multicultural company of 200,000 team members in over 40 countries. The Group reported 2017 global revenues of EUR 12.8 billion.
[1]Industry 4.0 is a name for the current trend of automation and data exchange in manufacturing technologies. It includes cyber-physical systems, the Internet of Things, Cloud computing and cognitive computing. Industry 4.0 creates what has been called a "smart factory".
[2]Capgemini's LifeSciencesPath solution is a predefined, SAP-qualified configuration based on Capgemini's experience in successful implementations; including its knowledge of industry-leading practices; and accelerated implementation methodologies and practices.
[3] SAP Manufacturing Execution (ME) on SAP HANA, SAP Manufacturing Integration and Intelligence (MII) and SAP(ERP)


text:
\section{Introduction}

Large scale cosmology is to leading order described by a Friedmann-Robertson-Walker line-element
\begin{eqnarray}
ds^2  = - dt^2 + a(t)^2 \left(dx^2 + dy^2 + dz^2\right)
\label{EQN_FRW}
\end{eqnarray}
with dynamical scale factor $a(t)$. Here,
the evolution of $a(t)$ is paramaterized by $H=\dot{a}/{a}$ and the deceleration parameter $q=-H^{-2}\ddot{a}/a$, where the dot refers to differentiation with respect to time. In evolving (\ref{EQN_FRW}) by general relativity, a dark energy density $\Lambda/8\pi>0$ is inferred from the observed three-flat cosmology with deceleration
\begin{eqnarray}
q=\frac{1}{2}\Omega_M-\Omega_\Lambda<0
\label{EQN_E1}
\end{eqnarray}
in Type Ia supernova surveys \citep{rie98,per99}. Here, $\Omega_M=\rho_M/\rho_c$ and $\Omega_\Lambda=\Lambda/8\pi \rho_c$, where $\rho_c=3H^2/8\pi$ denotes the closure density and $\Lambda$ is commonly referred to as a cosmological constant. The value $\Omega_\Lambda\simeq 0.7$ suggests that our cosmology is presently approaching a de Sitter state with a cosmological horizon at the Hubble radius $R=c/H_0$. A de Sitter state is fully Lorentz invariant, in our current Universe broken only by the presence of a minor amount of matter.

A telltale signature of dark energy in accelerated cosmological expansion (\ref{EQN_E1}) is its static or dynamic behavior. Here, we consider the problem of discriminating between $\Lambda$CDM and a dynamic dark energy in the form of $\Lambda=(1-q)H^2$, recently proposed as a back reaction of thermodynamic properties of the cosmological horizon \citep{van15b} motivated by holographic arguments \citep{bek81,tho93,sus95,van12} and a modified Gibbons-Hawking temperature \citep{unr76,gib77,cai05}. This dynamical dark energy has the property that it vanishies in the radiation dominated era, leaving baryon nucleosynthesis unaffected. In this era, the surface gravity of the cosmological horizon vanishes, when it touches the light cone of distant inertial observers. These two alternatives predict distinct values of the derivative $Q=\left.dq(z)/dz\right.$ at redshift $z=0$:
\begin{eqnarray}
Q_{stat}<1,~~~Q_{dyn}>2.5
\label{EQN_Q}
\end{eqnarray}
in $\Lambda$CDM and, respectively, $\Lambda=(1-q)H^2$. Illustrative for a holographic origin of $\Lambda$ is a dimensional analysis based on $L_0=c^5/G$ and the associated pressure $p=L_0c/A_H$ on the cosmological horizon, where $A_H=4\pi R_H^2$. In a pure de Sitter space $(q=-1)$, $\rho_\Lambda=-p$ by Lorentz invariance, whereby $\Omega_\Lambda=2/3$ in remarkable agreement with observations. See also \citep{eas11} for a derivation based on entropic forces.

By (\ref{EQN_Q}), $q(z)$ can be used to distinguish between $\Lambda$CDM and a dynamical $\Lambda$, provided it is resolved sufficiently accurately about $z=0$. Current data from Type Ia supernova surveys, however, seem inconclusive, that appears to be due to systematic errors possibly related to the tension with Planck data on the Hubble parameter \citep{pla13,pla14}.

Here, we consider a new probe of $q(z)$ in galaxy rotation curves and its implications for clustering of dark matter. This approach is based on a finite sensitivity of weak gravity to $\Lambda$ (static or dynamic). Gravitational attraction beyond what is inferred from (luminous) baryonic matter is generally observed in galaxies and galaxy clusters \citep{fam12} at accelerations of 1\,\AA\,s$^{-2}$ or less. This apparent non-Newtonian behavior is commonly attributed to dark matter, based on the success of Newton's theory of gravity in the solar system and its extension to strong gravity by embedding in general relativity. Supporting data for the latter derive from orbital motions at accelerations $a=R_g(c/r)^2\simeq  10^{-6}-10^{-2}$ m\,s$^{-2}$ of planets in the solar system at distances $r$, where $R_g = GM_\odot/c^2\simeq 1.5$ km denotes the gravitational radius of the Sun with Newton's constant $G$. Its extension in general relativity to higher accelerations has been fully vindicated by precession measurements in the Hulse-Taylor binary pulsar PSR1913+16 ($a=10^0-10^2$ m\,s$^{-2}$) \citep{hul75}. However, our observations of dark matter take us to the opposite limit of extremely weak gravity, not probed by our solar system or strong field counterparts in compact binaries. The parameter regime of about 1\,\AA\,s$^{-2}$ takes us away from existing tests of Newtonian gravity by a factor of about $10^4$, which is not small. Importantly, this scale is similar to the scale of cosmological acceleration $a_H=cH$, where $c$ denotes the velocity of light and $H$ is the Hubble parameter. Currently, $H_0 \simeq 67$ km s$^{-1}$Mpc$^{-1}$ \citep{pla13,pla14}.

To realize our new probe of $q(z)$, we consider weak gravity on the cosmological background (\ref{EQN_FRW}) parameterized by $(H,q)$ in a recent formulation of unitary holography
\citep{van15a}. In geometrical units with Newton's constant $G$ and the velocity of light $c$ equal to unity, $\Lambda$ and $\sqrt{\Lambda}$ are of dimension cm$^{-2}$ and, respectively, cm$^{-1}$, corresponding to dark energy volume and, respectively, surface density. The latter may be recognized as the thermal energy density $\Sigma = \frac{1}{2}T= {H}/(4\pi)$, defined by a de Sitter temperature $T_{dS}=H/2\pi$ \citep{gib77}. While $\Lambda/8\pi$ is notoriously small, $\Lambda \simeq 1.21 \times 10^{-56} \,\mbox{cm}^{-2}$, $\Sigma= \sqrt{\Lambda}/(4\sqrt{2}\pi) \simeq 6\times 10^{-29} \,\mbox{cm}^{-28}$ is not. An immediate implication is a critical transition radius for gravitational attraction. Around a central mass $M=M_{11}10^{11}M_\odot$ of a typical galaxy, $A\Sigma = M$ with for a two-sphere with area $A=4\pi r^2$, giving a transition radius
\begin{eqnarray}
r_t = \sqrt{MR_H} = 4.6 \,M_{11}^\frac{1}{2} \, \mbox{kpc}.
\label{EQN_rt}
\end{eqnarray}
The transition radius (\ref{EQN_rt}) is common to galaxy rotation curves and bears out in well in $a_t/a_H\simeq 0.1$ $(a_t = GM/r_t^2)$ in a deviation of centripital accelerations $a$ relative to the Newtonian acceleration $a_N$ expected from the observed baryonic mass \citep{mil83,fam12}, here shown in Fig. 1. (\ref{EQN_rt}) defines {\em strong} gravitational interactions in $r<<r_t$ and {\em weak} gravitational interactions in $r>>r_t$ with accelerations, respectively,
\begin{eqnarray}
a<<a_H,~~a>>a_H.
\end{eqnarray}
In geometrical units, holography hereby identifies $a_H$ as a critical acceleration in galaxy rotation curves.

\begin{figure}[h]
	\centerline{\includegraphics[scale=0.55]{plot_2}}
	\caption{Galaxy rotation curves (blue dots) reveal a transition to a $1/r$ force law at weak accelerations asymptotically in $a<<a_H$ away from Newtonian forces in $a>>a_H$ based on the observed baryonic matter. Shown is a theoretical curve (red) in unitary holography with a good match in a cosmological background with deceleration parameter close $q$ in the range $-1<q<-0.5$. Data are from galaxy curves with essentially zero redshifts from \cite{fam12}.}
\end{figure}

In \S2, we express gravitational attraction in terms of a conformal factor, encoding information on particle positions in unitary holography. The Newtonian limit is recovered in \S3, extended to non-Newtonian asymptotic behavior in $r>>r_t$ in (\ref{EQN_rt}) on a de Sitter background in \S4. A further extension to (\ref{EQN_FRW}) is given in \S5, wherein a finite sensitivity in $r>>r_t$ to $\Lambda$ is proposed as a new estimator for $q(z)$, proposed to determine (\ref{EQN_Q}).  We summarize our theory in \S6 with an outlook on future tests.

\section{Conformal factors from distance information}

Unitary holography expresses distances of particles of mass $m$ to time-like holographic two-surfaces in terms of information $I=2\pi \Delta \varphi$ defined by a total phase difference $\varphi=kr$ derived from its propagator with Compton wave number $k=mc/\hbar$, where $\hbar$ denotes the Planck constant. Holographic imaging is hereby an extension of holographic bounds originally developed for black hole spacetimes \citep{bek81,tho93,sus95} to spacetime outside black hole event horizons. Thus, $m$ is a holographic superposition of $A/l_p^2$ light modes determined by the hyperbolic structure of spacetime, where $l_p=\sqrt{G\hbar/c^3}$ denotes the Planck length.

This approach has two consequences. First, on macroscopic scales, $A/l_p^2$ is astronomically large. The holographic modes are extremely light with an energy scale
\begin{eqnarray}
\epsilon = \frac{mc^2l_p^2}{A},
\label{EQN_eps}
\end{eqnarray}
that introduces a sensitivity to any similarly low energy scale in the background vacuum. The latter is described by the elliptic structure of spacetime, that governs gravitational attraction. (In general relativity, the elliptic part embeds Newton's law of gravity in a conformal factor.) Second, holographic imaging is a function of $A\Omega$, where $A$ is the area of bounding surface and $\Omega$ is the projection opening angle of its surface elements. Factorization of $A\Omega$ is hereby an internal symmetry of holography \citep[cf.][]{tho15}. Scaling of $A$ and $\Omega$ corresponds to curvature and, respectively, lensing. These may be realized by a conformal factor or a deficit angle, that are essentially different manifestations of the same.

In encoding $I$ in $fA=A-A_E$ or, equivalently, $f\Omega = 4\pi - \Omega_E$, $A_E=8\pi ms$ and $\Omega_E=8\pi m/s$ are the Einstein area and opening angles, respectively, i.e.: $fA\Omega= 4\pi\left(A - A_E\right) = 4\pi A \left(4\pi - \Omega_E\right) = 16\pi^2s^2 f.$ Here, the factor of four in $A_E=4Il_p^2$ derives from a counting argument on the minimal number of bits required to encode matter and fields \citep{van15a}. A holographic screen hereby attains minimal size with $A=A_E$ or $\Omega_E=4\pi$ at the Schwarzschild radius $s=R_S$, $R_S=2m=\sqrt{S/\pi}$ with $S=\min I=4\pi m^2$ in $I = 2\pi m \left(s-R_S\right)+ S$ equal to the Bekenstein-Hawking entropy. Accordingly, we have
\begin{eqnarray}
f=1-\frac{2m}{s}.
\end{eqnarray}

In general relativity, the gravitational field about a point mass can be described by a conformal factor $\Phi$ in an isotropic line-element
\begin{eqnarray}
ds^2 = - N^2 dt^2 + \Phi^4\left(dx^2 + dy^2 + dz^2\right),
\label{EQN_A1}
\end{eqnarray}
where $N=N(\Phi)$ denotes the gravitational redshift, i.e., the ratio of energy-at-infinity to locally measured energy. According to the above, $R_S=\sqrt{4S/\pi}$ expresses the mass-energy of a particle by its linear size, locally measured by the minimal surface area $4S$ of an enveloping holographic screen. We are at liberty to choose a gauge
\begin{eqnarray}
N\Phi^2\simeq\mbox{const.},
\label{EQN_G}
\end{eqnarray}
defined by a constant total mass energy-at-infinity in the approximation of small perturbations to the spherically symmetric line-element (\ref{EQN_A1}). For a detailed consideration of such time-symmetric data, see \citep{van12}, where it serves as a condition in the application of Gibbs' principle in entropic forces in black hole binaries. According to the equations of geodesic motion, Newton's law then derives from $N$ in the large distance limit. With $dx^2+dy^2+dz^2= d\rho^2 + \rho^2d\theta^2 + \rho^2\sin^2\theta d\phi^2$ rexpressed in spherical coordinates $(\rho,\theta,\phi)$, $\rho$ reduces to the ordinary radial distance $r$ at large separations, (\ref{EQN_A1}-\ref{EQN_G}) embed Newton's law in
\begin{eqnarray}
\Phi \simeq f^{-\frac{1}{4}}\simeq 1 + \frac{m}{2r}~~(r>>2m).
\label{EQN_C}
\end{eqnarray}

\section{Newtonian limit in ordinary vacuum}

In what follows, unless otherwise specified, $A$ shall refer to surface area as well as the number of Planck sized surface elements $A/l_p^2$.

In holography, the wave function of a particle $m$ results from $A$ Planck sized harmonic oscillators of low energy (\ref{EQN_eps}). Ordinarily, one mode in the image appears for each mode in the screen. (The dimension of the phase space in the image equals the number of degrees of freedom in the screen.) Quantum mechanically, $m$ is the time rate-of-change of total phase as measured at infinity,
\begin{eqnarray}
m=\frac{1}{2}A\omega
\label{EQN_m}
\end{eqnarray}
of the ground state energies $(1/2)\omega$ of each harmonic oscillator in the screen. Distance encoding derives from aforementioned $\Delta\varphi = kr$ with the total wave number $k$ given by the superposition of these massless modes,
\begin{eqnarray}
k=\frac{1}{2}A\kappa,
\label{EQN_k}
\end{eqnarray}
based on the trivial dispersion relation $\kappa=\omega$ of ordinary vacuum, that recovers the Compton wave number $k=k_C$, $k_C=m$, with low energy frequencies
\begin{eqnarray}
\omega_N = \frac{2m}{A}=\frac{a_N}{2\pi}
\label{EQN_kN}
\end{eqnarray}
defined by the Newtonian acceleration $a_N={m}/{r^2}.$

The Compton relation $k=m$ recovered by the trivial dispersion $\kappa_N=\omega_N$ associates $\kappa_N$ with the Unruh temperature of Newtonian acceleration (\ref{EQN_kN}).

In entropic gravity \citep{ver11}, the above implies entropic forces on a test particle of mass $m'$ at screen temperatures $T=m/2\pi r^2$ by $dS=-dI = - 2\pi m' dr$, giving $F=-dU/dr=TdS/dr=-mm'/r^2$. In keeping with (\ref{EQN_G}-\ref{EQN_C}), however, we shall not pursue these arguments here.

\section{Sensitivity to $\sqrt{\Lambda}$ in a de Sitter background}

By (\ref{EQN_eps}), (\ref{EQN_kN}) is susceptable to low energy de Sitter temperatures of the cosmological horizon. Screen modes satisfy the dispersion relation
\begin{eqnarray}
\omega=\sqrt{\kappa^2+\omega_H^2}
\label{EQN_DR1}
\end{eqnarray}
representing an incoherent sum of a momenta $\kappa$ and the background de Sitter temperature, $\omega_H=T_{dS}$ \citep{nar96,des97,jac98}. A spherical screen imaging a mass $m$ at its center hereby assumes
\begin{eqnarray}
\omega_N=\omega-\kappa_H:~~\kappa=\sqrt{\omega_N^2+2\omega_N\omega_H},
\label{EQN_T1}
\end{eqnarray}
giving $\kappa\simeq \omega_N$ $(r>>r_t$) and $\kappa\simeq \sqrt{a_0a_N}$ $(r<<r_t)$ with $a_0=2a_H$ as proposed in \citep{kli11}. However, $\kappa(\omega_N)$ from (\ref{EQN_T1}) overestimates the Milgrom parameter $a_0$ \citep{mil83} by about {\em one order of magnitude} according to the data shown in (Fig. 1). Here, Milgrom's parameter is equivalent to the coefficient $A$ in the Tully-Fisher relation $V^4_c=AM_b$, where $V_c$ denotes the rotation velocity in a galaxy of baryonic mass $M_b$ \citep{mcg11a,mcg11b}. The wave number $\kappa_N$ in (\ref{EQN_T1}) is {\em not} representative for $\kappa$ of the image within.

On a background (\ref{EQN_FRW}) with $\Lambda>0$, image modes satisfy the dispersion relation
\begin{eqnarray}
\omega^\prime = \sqrt{\kappa^2 + \Lambda}
\label{EQN_DR2}
\end{eqnarray}
defined by the wave equation of a vector field in curved spacetime by coupling to the Ricci tensor $R_{ab}=\Lambda g_{ab}$. This applies to the electromagnetic vector potential \citep[e.g.][]{wal84} as well as the Riemann-Cartan connections in SO(3,1) in a Lorenz gauge \citep{van96}. It implies an effective rest mass energy $\sqrt{\Lambda}$ of the photon and graviton and photon. Effective mass is not the same as true mass. Even so, we mention in passing that the problem of consistent general relativity with massive gravitons has recently received considerable attention \citep{der11,ber14}. With $−q_0 H^2= H^2 + \dot{H}$ , the generalized Higuchi constraint $m^2 \ge 2(H^2 +\dot{H})$ \citep{hig87,des01,gri10} reduces to $\Omega_\Lambda\ge − 2 q_0$. Based on observations, $−1 < q_0 < −0.5$ \citep{rie04,wu08,gio12}, whereby $q_0 > -1$ appears secure at any rate.

By (\ref{EQN_DR1}) and (\ref{EQN_DR2}), distinct effective masses appear in the kinetic energies $E=\omega-\omega_H$ and $E^\prime=\omega^\prime - \sqrt{\Lambda}$ of low energy modes in the screen and image, namely
\begin{eqnarray}
E \simeq \frac{\kappa^2}{2\kappa_H},~~E^\prime \simeq \frac{\kappa^2}{2\sqrt{\Lambda}}
\label{EQN_O}
\end{eqnarray}
($\kappa<<\kappa_H,\sqrt{\Lambda}$). In weak gravitation in de Sitter space, therefore, {\em a direct correspondence between screen and image modes is lost}, in striking departure from the above Newtonian limit in $r<<r_t$ in the previous section.

Specifically, (\ref{EQN_O}) shows a discrepancy by a factor of $2\sqrt{2}\pi$ in effective mass $\sqrt{\Lambda}$ over that in $\kappa_H$. A given $\kappa=\kappa(\omega_N)$
of screen modes has an associated reduced energy in the relatively more heavy image modes, satisfying
\begin{eqnarray}
\omega_N^\prime=\omega^\prime-\sqrt{\Lambda}=\sqrt{\kappa^2+\Lambda}-\sqrt{\Lambda}
\end{eqnarray}
with corresponding reduced screen momenta $\kappa^\prime = \sqrt{\omega_N^{\prime2}+2\omega_N^\prime\omega_H}.$
Fig. 1 shows the graph $\kappa^\prime(\omega_N)$ to be in agreement with the data. Specifically, we arrive at Milgrom's constant
\begin{eqnarray}
a_0 =\left( \frac{\kappa_H}{\sqrt{\Lambda}}\right)2cH_0 = \frac{cH_0}{\sqrt{2}\pi} \simeq 1.5\times 10^{-8} \,\mbox{cm}\,\mbox{s}^{-2},
\label{EQN_a0}
\end{eqnarray}
where we restored dimensions in cgs units.

\section{Sensitivity to $q(z)$ in a FRW background}

The above generalizes to general Friedmann-Robertson-Walker (FRW) universes with modified de Sitter temperature \citep{cai05,van15b}
\begin{eqnarray}
T_{dS}= \frac{1-q}{2}\frac{H}{2\pi}.
\label{EQN_TdS}
\end{eqnarray}
\begin{figure}[h]
\centerline{\includegraphics[scale=0.55]{plot_4}}
\caption{Estimation of $q_0$ by a least-squares fit to the \cite{fam12} sample of low redshift galaxies shown in Fig. 1 following rescaling to various $H_0$ in units of km s$^{-1}$ Mpc$^{-1}$. The resulting correlation $(q_0,H_0)$ is agrees with Planck data on a relatively low Hubble parameter of about 67 km s$^{-1}$ Mpc$^{-1}$.}
\end{figure}
A key feature of (\ref{EQN_TdS}) is that $T_{dS}=0$ in the radiation dominated era $q=1$, whereby it pertains only to relatively late time cosmologies, satisfying
\begin{eqnarray}
\Omega_\Lambda = \frac{1}{3}(1-q),~~\Omega_{CDM}=\frac{1}{3}(2+q).
\end{eqnarray}

As a consequence of (\ref{EQN_TdS}), Milgrom's constant attains the explicit expression
\begin{eqnarray}
a_0 = \frac{\sqrt{1-q}}{4\pi}cH,
\end{eqnarray}
allowing measurement of $q$ from $a_0$ as a function of redshift:
\begin{eqnarray}
q(z) = 1 - \left( \frac{4\pi a_0(z)}{cH(z)}\right)^{2}.
\label{EQN_qa0}
\end{eqnarray}

The existing low redshift sample of galaxies of \citep{fam12} recovers the value $-1<q_0<-0.8$ for the Planck estimate of $H_0$ (Fig. 2) and is broadly consistent with Type Ia supernova surveys \citep{rie04,wu08,gio12}.

More detailed future observations of $a_0(z)$ about $0\le z <<1$ offer a new venue
for determine
\begin{eqnarray}
Q=2(1-q_0)^2-2(1-q_0)a_0^{-1}\left.\frac{da_0(z)}{dz}\right|_{z=0}
\label{EQN_dqda}
\end{eqnarray}
from a sample of galaxy rotation curves covering a finite range of low redshift $0\le z << 1$.

In \citep{van15b}, we considered the problem of discriminating between a dynamical and static $\Lambda$ parameter $(1-q)H^2$ versus $\Lambda$CDM. In the range of
$-1<q_0<-0.6$, Fig. 2 in \citep{van15b} shows the disjoint ranges
\begin{eqnarray}
 0<Q_{stat}<1,~~2.5<Q_{dyn}\simeq 2.8
\label{EQN_R1}
\end{eqnarray}
associated with, respectively, $\Lambda$CDM and $\Lambda=(1-q)H^2$.
Approximating the general trend in the first with $dq(z)/dz \simeq (5/3)(1+q_0)$
and the second with $dq(z)/dz\simeq 2.7$, Fig. 3 shows the correlation
(\ref{EQN_dqda}) with $a_0^{-1}da_0(z)/dz$ at $z=0$.
\begin{figure}[h]
	\centerline{\includegraphics[scale=0.55]{plot_5}}
	\caption{Shown are the correlations of $a_0^{-1}da_0(z)/dz$ with $q_0$ for a dynamical dark energy $\Lambda(1-q)^2H^2$ and a static dark energy in $\Lambda$CDM.
	In $-1<q_0<-0.6$, these correlations are sufficiently distinct to be discriminated observationally, provided that $a_0(z)$ is measured accurately over a small range of low redshifts.}
\end{figure}

\section{Conclusions}

In unitary holography of matter, conformal factors encoding positions and gravitation attraction have a hidden low energy scale (\ref{EQN_eps}), that introduces a finite sensitivity to low energy scales in the cosmological background (\ref{EQN_FRW}) parameterized by $(H,q)$. This sensitivity is manifest in a transition to non-Newtonian gravitational attraction, that scales with inverse distance beyond a critical radius $r_t$ at accelerations on the scale of the surface gravity of the cosmological horizon. It produces Milgrom's law with a specific expression for the $a_0$ as function of $(H,q)$. This $a_0$ sensitivity to $(H,q)$ may be probed observationally in low redshift galaxy rotation curves.

By agreeent with data shown in Fig. 1, there is no apparent need for clustering of dark matter on the scale of galactic disks. Even so, there exists a cosmological distribution of dark matter \citep{van15b}. A major conclusion of the present work, therefore, is that dark matter must be extremely light, giving clustering on the scales of galaxy clusters but not down to the much smaller scales of galaxies. Conceivably, the putative dark matter particle is the lightest element in the Universe and may not be readily detectable in a laboratory experiment based on interactions with ordinary matter.

We propose probing the static or dynamic nature of dark energy by $dq(z)/dz$. Values less than 1 or greater than 2.5 supporting $\Lambda$CDM, respectively, $\Lambda=(1-q)H^2$, here formulated in terms of $a_0^{-1}da_0/dz$ less than 2, respectively, greater than 2.5. These data may be obtained from an extended sample of low redshift galaxy rotation curves.

Finally, scaling of the transition radius (\ref{EQN_rt}) to laboratory test masses, $r_t \simeq 1\,\mbox{cm}\,M_0^\frac{1}{2}$ with $M=M_0$\,g suggests a possible laboratory test, probing the proposed sensitivity to the cosmological background by a space based free fall Cavendish experiment.

{\bf Acknowledgments.} The author gratefully acknowledges stimulating discussions with G. 't Hooft, D.M. Eardley, S.S. McGaugh and constructive comments from the referee. The author thanks the Kavli Instiute for Theoretical Physics, UCSB, were some of the work has been performed. This report NSF-KITP-16-016 was supported in part by the National Research Foundation of Korea and the National Science Foundation under Grant No. NSF PHY11-25915.

redpajama_set_name: RedPajamaArXiv


text:
Deze pagina geeft een overzicht van de wielerploeg Rabobank in 2001.

 Ploegleiders: Theo de Rooij, Adri van Houwelingen, Joop Zoetemelk, Frans Maassen, Nico Verhoeven, Jan Raas.
 Fietsenmerk: Colnago

Wielrenners

Overwinningen
 Brabantse Pijl - Michael Boogerd
Eindklassement Catalaanse Week - Michael Boogerd
3e etappe Tirreno-Adriatico - Markus Zberg
7e etappe Tirreno-Adriatico - Michael Boogerd
 Amstel Gold Race - Erik Dekker
 GP Eddy Merckx - Erik Dekker
6e etappe Ronde van Nederland - Erik Dekker
2e etappe Tour de France - Marc Wauters
8e etappe Tour de France - Erik Dekker
Eindklassement Ruta del Sol - Erik Dekker
 Wereldbeker - Erik Dekker
 GP van Frankfurt - Markus Zberg
13e etappe Ronde van Spanje - Beat Zberg

Teams

Ronde van Zwitserland
'''19 juni–28 juni
[11.] Beat Zberg
[12.] Markus Zberg
[13.] Grischa Niermann
[14.] Maarten den Bakker
[15.] Jan Boven
[16.] Marc Lotz
[17.] Geert Verheyen
[18.] Marc Wauters

Rabobank (wielerploeg)
Wielerploeg in 2001

redpajama_set_name: RedPajamaWikipedia


text:
using System;
using System.Collections;
using System.Collections.Generic;
using System.IO;
using System.IO.FileSystem.Tests;
using EnumerableTests;
using Xunit;

public class Directory_IEnumeratorTests : FileSystemTest
{
    private static EnumerableUtils s_utils;

    [Fact]
    public void runTest()
    {
        s_utils = new EnumerableUtils();

        s_utils.CreateTestDirs(TestDirectory);

        TestIEnumerator();
        TestClone();

        s_utils.DeleteTestDirs();

        Assert.True(s_utils.Passed);
    }

    private static void TestIEnumerator()
    {
        String chkptFlag = "chkpt_ienum_";
        int failCount = 0;

        IEnumerable<String> dirs_temp = Directory.EnumerateDirectories(s_utils.testDir, "*", SearchOption.AllDirectories);
        IEnumerator dirs = dirs_temp.GetEnumerator();

        try
        {
            if (!dirs.MoveNext())
            {
                failCount++;
                Console.WriteLine(chkptFlag + "1: MoveNext returned false. Expected some contents");
            }
            if (dirs.Current == null)
            {
                failCount++;
                Console.WriteLine(chkptFlag + "2: Current returned null. Expected some contents");
            }

            // Reset should throw
            dirs.Reset();
            failCount++;
            Console.WriteLine(chkptFlag + "3: Reset didn't throw exception. It should have thrown NotSupportedException");
        }
        catch (NotSupportedException)
        {
        }
        catch (Exception e)
        {
            failCount++;
            Console.WriteLine(chkptFlag + "4: Unexpected exception...");
            Console.WriteLine(e);
        }
        finally
        {
            ((IEnumerator<String>)dirs).Dispose();  // if we jump out while enumerating, the enumerator still holds the file handle
        }

        string testname = "IEnumerator";
        s_utils.PrintTestStatus(testname, "EnumerateDirectories", failCount);
    }

    // This testcase hits the FSEIterator's Clone method. Ensures that 2 different enumerators are returned and quick
    // functionality test.
    private static void TestClone()
    {
        String chkptFlag = "chkpt_clone_";
        int failCount = 0;

        IEnumerable<String> dirs_temp = Directory.EnumerateDirectories(s_utils.testDir, "*", SearchOption.AllDirectories);
        IEnumerator<String> dirs_enum_a = dirs_temp.GetEnumerator();

        dirs_enum_a.MoveNext();
        String da1 = dirs_enum_a.Current;
        dirs_enum_a.MoveNext();
        String da2 = dirs_enum_a.Current;

        IEnumerator<String> dirs_enum_b = dirs_temp.GetEnumerator();
        dirs_enum_b.MoveNext();
        String db1 = dirs_enum_b.Current;
        dirs_enum_b.MoveNext();
        String db2 = dirs_enum_b.Current;

        if (da1 != db1)
        {
            failCount++;
            Console.WriteLine(chkptFlag + "1: Enumerator A's 1st element ({0}) not equal to Enumerator B's 1st element ({1})", da1, db1);
        }
        if (da2 != db2)
        {
            failCount++;
            Console.WriteLine(chkptFlag + "2: Enumerator A's 2nd element ({0}) not equal to Enumerator B's 2nd element ({1})", da1, db1);
        }
        if (da1 == da2)
        {
            failCount++;
            Console.WriteLine(chkptFlag + "3: Enumerator A's 1st and 2nd elements are the same: {0}", da1);
        }

        // if we jump out while enumerating, the enumerator still holds the file handle
        ((IEnumerator<String>)dirs_enum_a).Dispose();
        ((IEnumerator<String>)dirs_enum_b).Dispose();

        string testname = "Clone";
        s_utils.PrintTestStatus(testname, "EnumerateDirectories", failCount);
    }
}

redpajama_set_name: RedPajamaGithub


text:
Splice Archive
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Cass Elliot - "Lady Love"
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The Unofficial Rules of College Sports Fandom
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Herzog, Hölderlin, and the Chauvet Cave
The Gold Standard of Dining
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The Baltimore Kid Does What He Feels
Remembering The Ass
Aug 06, 2016, 07:44PM
Nick(y)'s Picks Vol. 7
Nicky Smith
My personal favorite Pumpkins show ever.
This is my favorite Smashing Pumpkins performance ever. After six and a half years of voraciously consuming every bootleg, B-side, interview, and videos I could find, I keep coming back to this show. Twenty-two years ago today, The Smashing Pumpkins headlined Downing Stadium in New York as part of Lollapalooza 1994. There were two nights at Downing Stadium, and this is the second. The first night was a complete disaster. Listen for yourself: after giving Courtney Love time out of their set so she could play "Doll Parts" by herself, the Pumpkins took the stage and quickly careened way off course. Courtney's performance is remarkable, but the Pumpkins just completely fall apart for whatever reason. Five songs in, they launch into "I Am One," which had been expanded and bloated with a drum and bass vamp section in the middle so that Billy could rant and rave about the same things every night. You'd think he'd switch it up a little over the course of a year, but nope — at this point in 1994, diehard fans expected the "gimme gimme gimme gimme gimme gimme gimme gimme NOTHING" rant as much as the opening lick of "Today." It's high risk, high reward when all you've got going on stage is a rhythm vamp and Billy screaming at the audience for five minutes or more. On the first night, they lose all momentum during the rant section of "I Am One." Billy picks fights with audience members ("I don't take shit from nobody. Especially not a guy in a tank top and a mustache. I mean I'm not the best dresser, but you know…Tanktops are out, dude.") and goes way too far with the angry nihilist bit. The most powerful moment of the set is when Billy just loses it on some guy that told him to fuck off: "Yeah? FUCK YOU TOO, YOU FUCK. FUCK YOU, FUCK YOU, FUCK YOU!!! You can give me the finger, you can call me an asshole, I DON'T FUCKING CARE!!!!!"
People that were there can attest to how badly the band alienated the crowd that night. I know someone who was there on the first night that hasn't listened to the Pumpkins since because of their behavior that night. After "I Am One," the soldier on, before abandoning "Siva" halfway through and cutting the set early with a defeated cover of Thin Lizzy's "Dancing in the Moonlight." Exactly halfway through the forty-five date Lollapalooza tour, the band imploded on stage in front of a major market. Despite all their differences, the original lineup excelled when their backs were up against a wall and they had to prove themselves. This self-imposed pressure could backfire and occasionally resulted in disastrous shows, like their performance at the Reading Festival in 1992: Siamese Dream was still a year away, and the Pumpkins' were still deep in the shadow of Nirvana. Playing a daytime set at the same festival that Nirvana famously headlined, Billy felt they played so badly that he should break up the band. Rough festival sound aside, that doesn't show on the recordings I've heard — but it's impossible to ignore on the August 5, 1994 bootlegs. They fucked up.
So this is the scene on August 6: after an abysmal first night, the band come out eager to prove themselves and annihilate the audience. One of the most striking things about this show is that they open with "I Am One" — common during the Gish tours, but as far as I know, this is the only time they did it during the Siamese Dream tour. Instead of coming back with their tails between their legs, they open with their most challenging and atonal song, radically transformed from its original arrangement into a thrash metal spectacle. The main riff (F# to A) is played palm-muted and mimics the rat-tat-tat of rifle fire and goose-steps — this is also most likely the origin of the main riff in "Fuck You (An Ode to No One)." The difference between the two nights is obvious immediately: this is an anger focused, a controlled intensity that came with all of the band's best performances. Despite coming on — at least psychologically — as the defeated and embarrassed underdog, opening the show with "I Am One" is a gesture that gives the audience no quarter, and demands that the band be accepted on its own confrontational terms. It's a glorious and triumphant moment, and more than anything, that's what makes this my favorite Pumpkins bootleg: the spirit and the heart of the band is at stake and ultimately validated by a much more receptive audience. "We are The Smashing Pumpkins," Billy declares three songs in, "We always have been and always will be The Smashing Pumpkins. Some people like that, and other people don't. But that's okay, too."
Staples of the Siamese Dream tour make up most of the setlist, but the whole performance is just blistering, a supernova even outside the context of the night before. There is one other notable thing about the setlist, besides the "Bye June" tease in the middle of "Silverfuck" — Billy closes the show by singing "Sweet Sweet" a-cappella after the rest of the band have already left the stage. To date, it's the last time "Sweet Sweet" has ever been played live. Here and there on the fourteen-month Siamese Dream tour, Billy would occasionally close with this, to mark the end of a particularly stellar show. After a string of performances in March and April, "Sweet Sweet" wouldn't appear again until this show. It's clear by the end of the night that the Pumpkins have won — they captured the attention and enthusiasm of a crowd that was listless and often hostile the night before. Billy earnestly asks "Are you sure you're into this?" before "Hummer." The crowd erupts and affirms the band's success and he smiles from ear to ear, and despite his best efforts to remain as pissed off and malcontent at the time, Billy can't stop grinning and posing for the rest of the set. He even makes fun of his dour persona before "Starla," asking the crowd to "Please tell your parents we said hello. We do love parents. My parents died in a car crash…I can't tell them hello." With "Sweet Sweet," they end as strongly as they began, with a few parting words from Billy: "One more thing. When I started singing this song, I heard somebody yell, 'Oh, it's another one of them songs about love.' Well, yes it is, and I'm going to keep singing them forever, too."
I Am One (with rant)
Cherub Rock
Geek U.S.A.
> The Sign [Ace of Base]
(tease)
Silverfuck
> Bye June
(tease) > Over the Rainbow [Harburg/Arlen] (tease)
Sweet Sweet
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text:
//-----------------------------------------------------------------------------
var UBound = 0;
var bug = 39309;
var summary = 'Testing concatenation of string + number';
var status = '';
var statusitems = [];
var actual = '';
var actualvalues = [];
var expect= '';
var expectedvalues = [];

function f(textProp, len)
{
    var i = 0;
    while (++i <= len)
    {
       var name = textProp + i;
       actual = name;
    }
}

status = inSection(1);
f('text', 1);  // sets |actual|
expect = 'text1';
addThis();

status = inSection(2);
f('text', 100);  // sets |actual|
expect = 'text100';
addThis();

//-----------------------------------------------------------------------------
test();
//-----------------------------------------------------------------------------

function addThis()
{
  statusitems[UBound] = status;
  actualvalues[UBound] = actual;
  expectedvalues[UBound] = expect;
  UBound++;
}

function test()
{
  enterFunc('test');
  printBugNumber(bug);
  printStatus(summary);

  for (var i=0; i<UBound; i++)
  {
    reportCompare(expectedvalues[i], actualvalues[i], statusitems[i]);
  }

  exitFunc ('test');
}


text:
Z House Stories
All About Reading To Children
For Parents & Kids
How can a map of tech-assisted interventions in early literacy be helpful?
Posted by Holly on July 4, 2015 Leave a Comment
Technology tools sit at our kitchen table, ride with us in our car, and take a place on our bedside table. Smartphones, tablets, TVs with video games, and computers are turned on ─and we're tuned in, adults and children alike.
These developments are not lost on educators. Shayna Cook who studies an array of policy issues concerning birth through third grade for New America's Early Education Initiative recently noted that: "Many early education programs around the country are beginning to determine how they might harness these [technology] tools to engage with parents, improve home-to-school connections, and otherwise augment efforts to help children develop early language and literacy skills."[1]
Cook describes an interesting new effort led by New America and the Joan Ganz Cooney Center at Sesame Workshop ─ the launch of an interactive U.S. map of early literacy programs categorized into five buckets:
Professional learning programs
Center and school initiatives
Home visiting and parent engagement programs
Library and museum programs
Public media partnerships.
The just-released "beta" version of the interactive map lets you click on "pin-drops" categorized by these five types of programs. What you get when you click on the map is information about the literacy program; for example, where the program is located, what tech tools are used, and what evidence of impact there is on children's reading skills through the program's intervention. Each program provides information within the following 14 categories:
Story of program beginning
Technological tool(s)
Purpose of technology
Technology concerns
Biggest challenges
Program documentation
Evidence of impact
Evidence of impact rating
Larger initiative
List of program partners
For example, when you click on the pin-drop positioned in central Ohio, up comes "Kids Read Now" which targets children ages 6-8 and is categorized as a center/school initiative. The description tells us that this program "seeks to eliminate the summer reading slide[2] by partnering directly with schools to enroll students in grades K-3. Students choose nine books, attend a Family Reading Night event where they receive the first three of those books, and then receive weekly phone calls/text messages/emails throughout the summer to remind them to read their books. These calls, placed using One Call Now technology, allow students to record books they have finished. When a book is reported as finished, the child is sent another book from his/her list through the mail. Children keep all books."
While this program is available nationally, the statistics seem to come from Ohio and Indiana: "During summer 2014, we enrolled 4,000 students from 22 school buildings in Ohio and Indiana in this program. We estimate our program will serve approximately 5,000 students from 24 buildings during summer 2015. We have hopes of growing to serve a national audience and are limited only by the amount of funding we have in place."
When you click on the pin-drop in New Mexico, up comes the "Great Reading Adventure" which is in the library/museum category. This is "an online platform to help families engage in the statewide summer reading program and track minutes read over the summer. [The] online platform allows participants to earn badges and complete early literacy activities as they participate in the summer between May and August." Serving more than 10,000 students, the technology tools the program uses are touchscreen tablets, mobile apps, and computers online. The program is finding "a way to make it easier for families to engage and participate in the summer reading program by using technology to help overcome common issues or challenges such as transportation or lack of access."
The challenges identified by the 28 programs on the U.S. map are interesting. For example, New Mexico's program cites the lack of or unreliable internet access, lack of professional development (presumably for librarians and other staff), and concern about using technology with families with young children (see other Z House blogs on research calling for limits on "screen time" for very young children). The Ohio program cites lack of access or transportation as a challenge.
The name of the mapping project is "InTEL: Integrating Technology in Early Literacy." Early feedback on InTel is promising ─ the map-makers report "positive feedback from state and program leaders who have been testing new approaches and need to be able to see the landscape and find examples with a solid research base."
This map is really for an "inside baseball" audience ─ state and program leaders and researchers in early child literacy. This is not a map that seems to be designed for parents, teachers, librarians and others on the frontline working with children to improve their reading skills. But the map could in my view morph into a source of useful information for a frontline audience as the map is improved in the coming months and years. It may be useful, for example, to know what programs are operating in your schools, libraries and museums; and what programs are out there in other communities that would be helpful to adopt/adapt for your community to fill gaps in literacy programs for children.
Efforts are underway to improve the map. The current pin-drops were fed by data collected from a national survey conducted in February 2015. The survey has been re-opened to collect more information. So the good news is the InTEL map-makers will continue to update and expand the pin-drop sites. More good news would be expanding the use of the map ─from the "inside baseball" audience to the "frontline" audience who could help call for the adoption and adaptation of well-tested early literacy programs.
Would that the "pin-drops" become so numerous on the U.S. map that the map-makers biggest challenge is how to portray them!
[1] "A Map in Progress: Integrating Technology in Early Literacy" (June 15, 2015): http://www.edcentral.org/beta-map-intel/
[2] "Slide" refers to students who lose their reading skills during the summer.
Filed Under: Author Musings/Reflections, Informed by Research, Literacy News | Tagged: Tagged With: technology-integrated literacy; tech-assisted early literacy and language development; InTL; early literacy; reading improvement
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Wonderful news for the Zone! A thank-you letter from Johnny Depp!
Re: Wonderful news for the Zone! A thank-you letter from Johnny Depp!
Gilbert's Girl wrote: Modest as usual, lovely.
Do you get sent the physical letter by mail or do you get it by e-mail, just curious?
I realized I was so excited when I was reading the initial Zone responses that I neglected to answer your question.
In the early days, when we first started doing our Birthday Projects, I would receive a physical letter in the mail (only).
For the past couple of years, including this one, I have received an email with Johnny's letter attached very soon after the Birthday Project closed, with a hard copy of his letter following in the mail to me a little while later.
I received the actual letter from Johnny by Federal Express to my door today, which reminded me that I owed you an answer. I post the letter as soon as I receive it by email, however, since I don't think Zoners should have to wait for the news.
Once again, this is just such a lovely place. The sincerity of all the principals, the humanity of the actor whose work we so appreciate. The whole thing just moves me to tears, as silly as that may sound. It's really as though we all lived around the corner from each other. I don't think it will ever stop surprising me.
I know it's a UPS smilie instead of Fedex, but did you do this when the letter came, PTP?
Yup! And I'm still smiling.
part-time poet wrote: In the early days, when we first started doing our Birthday Projects, I would receive a physical letter in the mail (only).
What a lovely note of appreciation! It shows what a truly warm and caring person Johnny is; that along with his generosity in supporting this very worthy cause shows how sincere he is in his feelings towards Native Americans. God bless him! I am proud to be a Johnny Depp fan and a member of this family of Johnny Depp fans and supporters.
Thanks PTP for getting back to me on that So do you frame it?
Just wanted to give an update on the water systems project. We had 3 interns on site over the past few weeks, and they were able to gather the details from each families house, figure out the exact parts (some families already had some parts), and put the orders in. As a result of their diligent work, we were able to include an extra family - that's 6 families instead of 5!
The systems should be going on shortly as the materials are on route to each families homesite.
Again, none of this would've been possible without your kindness - thanks again!
Thanks so much for the update, Sean.
Location: Hiding under the tree tops.
This is amazing news !! Thank you so much for the update.
I am completely moved by all the work that goes into this.
For those that are out there putting in the people power to get this up and running. For without their work/time/effort this task would not be complete.
This is wonderful news! Thank you, Sean for the update.
I can see I have been spending too much of my web time on Facebook. There's so much fun here. I am going to start dividing my web time between here and Facebook.
RamblinRebel wrote: Six families! YES!


"Leviathan" redirects here. For other uses, see The Leviathan Skin.
The Leviathan Mouse is a breed of mouse found on the ship the S.S. Huntington IV. They are known to drop Simple Orbs as loot. They are also known to drop Mesh Netting as loot, but only while hunters are in the process of completing the Zurreal Trap Research Assignment.
Leviathan mice have no specific preference for any kind of cheese.
On 25 January 2011 they began to drop Simple Orb as loot.
On 23 August 2011 they began to drop Mesh Netting as loot.
This page was last edited on 2 January 2019, at 13:24.