OpenLLM-France/wikimedia huggingface dataset:
# Handbook of Genetic Counseling/Bardet-Biedl Syndrome-1

Bardet-Biedl Syndrome

## Introduction

* How have thing been going since we saw you last?

## Contracting

* Are there some major issues that you want to make sure are addressed today?
* We will gather medical information, any changes in the family, physical exam

## Interim History

* Hospitalizations?
* Surgeries?
* Illnesses?
* Any doctor visits?
* Ophthalmology visit?
* How's the eating schedule been going?
** Regular meal times?
** Modified meals?
** Scheduled snack times?
** Restricted to one helping at meals?
* Is involved in any school-type programs?
** EI preschool referral
* Behavior issues
* Developmental issues
** speech difficulties?
** Motor issues (walking, running)
** Know colors/body parts
** Potty trained

## Establish Plan

* Reiterate plan that was agreed upon in case (i.e. hospitalization in two weeks time? Vs. continue with strenuous weight loss plan)
* Reassess parents' state of mind and emotional level
* Make sure parents understand importance and necessity of 1) eye appointment & 2) weight loss

## Notes

The information in this outline was last updated in 2000.
# General Astronomy/Solar Activity

Sunspots are caused by magnetic disturbances that erupt through the visible surface of the Sun (photosphere). Deep inside the Sun many free moving subatomic particles produce very strong and complicated magnetic fields. When strong magnetic field lines erupt through the photosphere, they slightly impede the flow of energy from deeper layers outward to the surface, thus causing the area of the sunspot to be slightly cooler than the rest of the Sun, and hence darker.
Sunspots typically have a dark inner zone called an umbra, surrounded by a lighter outer zone called a penumbra. Many are as large as the Earth, and some have been known to be as large as Jupiter. Larger sunspots are usually groups of spots rather than just one. Often, adjacent sunspots have been shown to be of opposite magnetic polarity, with magnetic field lines flowing from one to the other, much like a bar magnet.
The solar activity cycle corresponds to the sunspot cycle, and is on the average about 11 years. That is, the numbers of sunspots, along with other less obvious activity on the Sun, waxes and wanes about every 11 years. In addition, the magnetic polarity scheme of sunspots reverses once every cycle, so we can also say that there is a 22-year cycle in solar activity.
# General Astronomy/Supermassive Black Holes

The general consensus today is that when galaxies form, the phenomenal concentration of matter at their cores leads inevitably to the formation of "supermassive" black holes (SMBH). Unlike a "normal" black hole that forms from stars only a little more massive than our Sun (stellar mass black holes), "supermassive" black holes range from hundreds of thousands to perhaps a billion or more times the mass of our Sun.
Contrary to image in movies and the media, black holes do not "suck" everything in and it is perfectly possible for stars and gas clouds to orbit around a black hole without being pulled in or destroyed. In fact, observations of the very rapid motions of stars near the center of the Milky Way have given the first proof that such a monster lurks at the heart of our own Galaxy. The stars in this region are orbiting a common center, and their very fast motions indicate an extremely strong gravitational attraction at that point. Using Newton's version of Kepler's laws, astronomers have determined that this mass is the equivalent of about 4 million times the mass of our Sun. Since there is no light or other radiation coming from this point, we reach the inevitable conclusion that it is a supermassive black hole.
Other evidence strongly suggests that similar SMBHs exist in the cores of most if not all other galaxies. Ours is quiet or quiescent today, but not so in some other galaxies.
# General Astronomy/Star Clusters as Cosmic Laboratories

It is estimated that the number of the stars in the universe is around $10^{20}$. This is calculated based on the fact that there are about $10^{9}$ galaxies in the universe, each of which is composed of an average of $10^{11}$ stars each.
A nebula is a cloudlike object. Scientists can determine what type of nebula they are observing by examing its spectrum: an emission spectrum indicates glowing gas, while an absorption spectrum indicates a mass of stars. The Pleiades, for instance, has absorption spectrum.
Two kinds of nebulae are open clusters (loose groups of a few hundred stars; e.g. Pleiades, Hyades, Ursa Major) and globular clusters (spherical nebulae with hundreds of thousands of stars, such as M13 in Hercules and M3 in Canes Venatici). Most nebulae appear as a hazy patch when viewed with a small telescope. Dark nebulae are gaseous clouds that block light. This is where stars form.
Stars are created when gravity collapses dust and gasses together.
# General Astronomy/Space Weather

Space weather is a general term that applies to the environmental conditions in space imposed largely by solar activity such as the "wind" of subatomic particles that constantly flows from the Sun. This Solar wind sometimes rages into a "storm" of charged particles (mostly electrons and protons) that can affect, disturb or even incapacitate satellites in orbit, disrupt communications, and pose radiation danger to unprotected astronauts.
The best known aspect of space weather is the aurora, commonly known as the "Northern Lights" in the Northern Hemisphere, with the corresponding "Southern Lights" in the Southern Hemisphere. These are formally known as the Aurora Borealis and Aurora Australis, respectively. they occur when large masses of the charged solar wind particles are attracted to the polar regions by Earth's magnetic field. As they spiral down through the atmosphere, they collide and interact with molecules in the atmosphere, most notably nitrogen and oxygen, which causes the emission of light seen as the aurora. The process is similar to that in an fluorescent light.
During particularly intense solar wind storms, electrical charges can collect on electrical transmission lines on Earth, sometimes causing an overload and blackouts (such as in Quebec in 1989). In addition to affecting the radio characteristics of the upper atmosphere, the solar wind charges also collect on orbiting communications satellites and can disable them unless precautions are taken. It is estimated that a solar storm of the intensity of the one in 1859 were to strike it could cause up to 2 trillion dollars damage.
Potentially more deadly are X and Gamma rays that can harm astronauts on flights well away from Earth, such as to the Moon or Mars. Space Shuttle and International Space Station astronauts are at only moderate danger since the Earth's magnetic field provides some partial protection for astronauts in low-Earth orbits (as both the space shuttle an ISS are).
# General Astronomy/Spaghettification

Spaghettification refers to the effect of extreme gravitational pressure on any particle or body of matter, in particular when exposed to the extreme forces of the black hole. Essentially, when a particle draws too close to the source of the powerful gravitational field, it is stretched into long thin shapes, like pasta.
The term was coined by Stephen Hawking in his book, A Brief History of Time, where he likened this process to spaghetti. Much like other aspects of the black hole theory and model, this effect of drawing too close to a black hole remains untested, unobserved and unproven, and relates to areas of physics that remain largely unexplored, namely the concept of a force so powerful that no matter what components make up a piece of matter, it will be stretched further than is deemed by many to be within the realms of physical plausibility.
Many have speculated upon why it is, scientifically speaking, that spaghettification occurs when an object draws close to a black hole, but a generally accepted theory has been proposed. To understand this, one must consider the sheer strength of an object with such a high gravitational pull. One must also consider Newtonian gravitational theory, which states that:
* If you increase the mass of an object within a gravitational field, the gravitational pull in question will increase in power by the same amount.
* These factors become exponentially higher as the object draws closer to the source of the gravitational strength.
Bearing that in mind, one now must consider that:
* Black holes have extremely high masses, often many times that of the sun and other stars
* This mass is concentrated in a very small radius.
* Because of these factors, the gravitational force near a black hole is enormous...
* And all the above factors thereby contribute to the largeness of the gradient of the gravitational field across the object within the field as it draws closer and closer to the source.
Effects of this on the article in question are extreme. Spaghettification tears at the matter's very atomic structures, elongating them and stretching them until they are atomically and cellularly unrecognisable.
Spaghettification is also largely based on the positioning of the object, and the trajectory at which it approaches the source of the gravitational power. These factors cause variations on the way the gravity acts on the incoming matter, and spaghettification is caused based by the differences in the forces fronting the object in question.
# General Astronomy/Telescopes/Basic Optics

Although the Greek origin of the word telescope means far-seeing, "see something far away" is not a good description of the function of a telescope. If an object is bright enough, no matter how far it is, we can see it. In fact, telescopes serve three main functions:
* light collection
* resolution
* magnification
Before understanding how telescopes work to achieve these three goals, we take a pause here and study some principals that the optics work.

## Reflection and Refraction

The most primitive type of a telescope is a refracting telescope (also called a refractor), which is used by Galileo back in the 1600s. Later, Newton designed and built a reflecting telescope (also called a reflector) making use of mirrors. We first focus on refracting telescopes. A basic refractor consists of a converging lens which focus light onto the focal plane at which detectors and instruments are then placed. As discussed in the previous chapter, the path a light ray passing through a lens can be understood by the Snell's law of refraction:
$n_{1}\sin {\theta _{1}}=n_{2}\sin {\theta _{2}}\,.$

## Magnification

Magnification in a telescope can be given by the following formula: mag=focal length of the objective lens÷focal length of the eyepiece lens

## Light Gathering Power

Since most objects in the sky are very dim, a telescope effectively collects and converges light for our viewing. How dim are they? A brief calculation helps explain.
The Sun is at a distance of 1 AU (~1.5e+11 m) away, the light coming out "spread" over a spherical surface (actually it is the energy that spreads over a surface, which we call the flux). Suppose we have a telescope with a 2 m (diameter) aperture, then the fraction of light collected from the Sun is
    ${\frac {\mbox{light collecting area}}{\mbox{area of spherical surface}}}={\frac {\pi (1)^{2}}{4\pi (1.5\times 10^{11})^{2}}}\simeq 1.1\times 10^{-23}\,.$
For objects beyond the solar system, they are millions, if not billions, times further away from us. Therefore, astronomers prefer to build larger telescopes for greater light collecting power.
# General Astronomy/Telescopes/Optical Telescopes

Optical telescopes increase the apparent brightness and magnification of an object. Other telescopes are capable of "seeing" in the electromagnetic spectrum beyond the abilities of our eyes and transforming those images to those we can use. Infrared telescopes are capable of detecting heat signatures. There are also huge radio telescope dishes, as well as ultraviolet and x-ray telescopes that have been launched into orbit beyond the our Earth's obscuring atmosphere.
There are two main types of optical telescope - reflectors and refractors. Reflectors use a mirror to collect the light, whilst refractors use a lens. Generally, reflectors are better for deep sky objects whilst refractors are useful for planetary observations. Some telescopes use a combination of lenses and mirrors to use the advantages of each.
Refractor telescopes require a large lens at the front to direct the incoming light to the lens. This lens may be made of more than one piece, and the differing refractive properties of the components serve to reduce aberration at the edge of the image. The lenses may also be coated to reduce internal reflections.
Catadioptrics are short, wide telescopes that use both mirrors and lenses.
Large lenses suffer sag under their own weight. This causes their shape to become distorted and so the image will be irregular. For this reason the largest refracting telescope ever built only has a diameter of 41". All larger telescopes, instead, use a mirror as the primary collecting surface.
In the optical spectrum, great precision is required in crafting the lenses and mirrors used in a telescope. The standard of precision for a telescope mirror is accuracy to 1/4 the wavelength of light, an exceedingly small quantity. But even greater accuracy is generally preferred, especially for space-based telescopes. Special tools have been developed for measuring the accuracy of a telescope mirror and lens, and the procedure for finishing the surface is very exacting.
# Haxorware Modem Firmware/Config File
## Force Config File

Server IP This is the IP address of the TFTP server hosting the config file you want to run.
File name This is the filename of the config file you want to pull from the above IP

## Autoserve

Autoserve Config File Disabled until new config is uploaded. Some ISP's can be tricked to allow you online using a config file saved directly to your modem instead.
Store new config Where you upload a stored config file.
# Haxorware Modem Firmware/Frequency

Annex - Choose DOCSIS or EURODOCSIS based on your region. Plan Choose the type matching your region. Preferred DS Freq 1, 2, & 3 is displayed in "Hz" not "mhz" (for example - 600mhz would actually be entered as 600000000) These are the frequencies checked first before scanning.
Upstream Channel This is the preferred upstream channel to try before scanning for available channels.
# Haxorware Modem Firmware/Configuration Settings
## settings

Factory Mode This forces the modem to behave as if it was supplied by the ISP and bypasses customs settings. Disable Firmware Upgrades This option will force Haxorware to ignore new modem firmware pushes from the ISP. Unchecking this could compromise your Haxorware install. Force Network Access No information available at the moment.
Tftp Enforce Bypass If your ISP enforces Tftp config file this option will tell the modem to download the supplied config file at the right point - even if you are using another one.
Disable IP Filters on startup IP filters are used by some ISP's to block traffic of certain types on certain ports (such as if your ISP blocks port 80 to prevent you from hosting a web server). This option bypasses them entirely.

## Timeouts

Ignore T1 (No valid UCDs)
Ignore T2 (Ranging Opportunity)
Ignore T3 (Ranging Response)
Ignore T4 (Station Maintenance)

## Administration

Control Panel IP Address Set a different IP than standard here if necessary DHCP Server Check this to assign the IP to WAN on router or to PC. Uncheck this ONLY if you have it set manually.

## WebGUI

Password protection enable or disable Password protecting the GUI from tampering.

## Telnet Server

Current state Whether Telnet services are running Run on startup Whether Telnet should start when the modem is booted, or only when manually enabled.
# Haxorware Modem Firmware/Installation

Installation varies based on your available method. Some methods require different hardware modifications such as a Jtag or serial connector (outside the scope of this wiki) ALWAYS backup current firmware. If you flash a 2mb dump over the existing firmware you will lose the modems original certificates forever.

## JtagUtility Instructions:

If your modem is currently running infinite firmware it is recommended to restore it to stock, like it was out of the box. To do this you restore your 2MB backup that i hope you made before flashing infinite. The commands are as follows:
It is recommended you make a backup before flashing haxorware (or any other hacked firmware) onto your modem. To create a 2MB backup with JtagUtility, enter the following commands:
To program haxorware to your modem using JtagUtility, issue the following commands:
After the flashing is complete, reboot your modem and enjoy Haxorware

## Flashing over serial:

Diagnostic cable instructions (requires noisy bootloader):

## USBJTAG Instructions:

If your modem is currently running infinite firmware it is recommended to restore it to stock, like it was out of the box. To do this you restore your 2MB backup that i hope you made before flashing infinite. The commands are as follows:
It is recommended you make a backup before flashing haxorware (or any other hacked firmware) onto your modem. To create a 2MB backup with usbjtag enter the following commands:
To program haxorware to your modem using USBJTAG, please overwrite your usbjtag.def with the one from this archive. After that, start USBJTAG and choose the SB5101 profile (Tools->Config will open the profile selection dialog) Then issue the following commands:
After the flashing is complete, reboot your modem and enjoy Haxorware

## USBJTAGNT Instructions:

If your modem is currently running infinite firmware it is recommended to restore it to stock, like it was out of the box. To do this you restore your 2MB backup that i hope you made before flashing infinite. The commands are as follows:
It is recommended you make a backup before flashing haxorware (or any other hacked firmware) onto your modem. To create a 2MB backup with usbjtag enter the following commands:
To program haxorware to your modem using USBJTAGNT Start USBJTAGNT and choose the SB5101Mod profile (Tools->Config will open the profile selection dialog) Then issue the following commands:
After the flashing is complete, reboot your modem and enjoy Haxorware
USBJTAG NT is just Li Shao's way to get more money out of users by planned hardware obsolescence (otherwise the USBJTAG NT software would support the regular USBJTAG as well).

## Upgrading from previous shelled firmware (infinite) or Haxorware 1.0

Haxorware 1.1 should now boot
# Haxorware Modem Firmware/Firmware upgrade
## Firmware upgrade

Firmware Image Pick the file you want to upload. Be sure to pick the right one. Haxorware DOES however have provisions to prevent drastically wrong choices (such as accidentally picking a 10kb text file)

## Bootloader upgrade

Bootloader Image Update the bootloader only (such as if you need to load the noisy bootloader to diagnose issues)
# Haxorware Modem Firmware/Overview
## HFC Parameters

Mode DHCP assigned address or Static IP Address Your currently assigned IP address
Subnet Subnet mask applied to your IP address
TFTP Server "Provisioned" Config file name assigned by your isp
TFTP Filename “Provisioned" Config file name assigned by your isp
ToD Server "Provisioned" Time Of Day server IP assigned by your isp to synchronize against.
Configuration file Name "Actual" Config file name in use. when using one different from what was assigned by the ISP the filename shows here.
Size Config file size
'Compliance ' DOCSIS version compliance of this config file.
# Haxorware Modem Firmware/Signal
## Downstream

Frequency This is the frequency your downstream channel is on
Status Whether the channel is locked or in process Annex DOCSIS or EURODOCSIS Modulation Modulation rate such as QAM256, QAM16, etc. Higher is faster. Symbol Rate Number of symbols per second.
Receive Power Downstream channel signal strength measured in dBmV. Signal to Noise ratio SNR measured in Decibles (Higher is better)

## Upstream

Frequency This is the frequency your upstream channel is on Channel ID Upstream channel number Status Whether the channel is locked or in process Mode TDMA or ATDMA. (ATDMA is faster) Symbol Rate Number of symbols per second.
Transmit Power Broadcast signal strength to the head end at your ISP measured in dBmV
# Haxorware Modem Firmware/Baseline Privacy
## Baseline Privacy

BPI Baseline privacy version running. BPI 1.1 must be enabled to use docsis 1.1 config files with valid certificates. Bypass must be enabled to use 1.1 configs with self signed certificates but will not work on all providers

## Backup/Restore

Backup Backup your current certificate set
Restore from filesystem Restore uploaded or previously backed up certificate sets Restore from file

## Certificate Download

CertificateDownload individual certificates

## Certificate Upload

Upload individual certificates here
# Haxorware Modem Firmware/Downloader

This page allows you to download config files from your ISP's TFTP server to examine them with programs such as vultureware or autoserve them from the modem.
The IP address and Filename may be entered here, and clicking download will prompt you with a file save dialog box.
# Haxorware Modem Firmware/File Manager

File System info

## Free Space

Before Defragmentation Size in KB before a defragmentation is performed
After Defragmentation Size in KB after a defragmentation is performed

## Haxorware Configuration

Config File This allows you to Download or Delete the existing config file stored in the modem File Size Filesize of config file in Bytes
Entries Number of entries in the config file

## Restore From File

'Files' Previous backup files or uploaded files are shown here which can be downloaded or deleted in the following format:
CMXXXXXXXXXXXX.tar (size in bytes) (option)Download Delete

## Upload New File

Choose file dialog prompted when this is clicked. Click upload after picking file to upload
# Dark and Light/Skills/Warrior

* Weapon Abilities
* Cries Abilities
jump to Fighter Skills jump to Citizen Skills
back to Warrior Class
# Dark and Light/Skills/Wizard

jump to Mage Skills jump to Citizen Skills
back to Wizard Class