text:
Eye of Cthulhu
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vEye of Cthulhu4 | ||
Stats | ||
Type | Monster | |
HP | 1st Phase: 2800 2nd Phase: 1400 | |
Attack | 1st Phase: 15 2nd Phase: 23 | |
Defense | 1st Phase: 12 2nd Phase: 0 | |
Variety | Demon Eye The Twins | |
Spawn Time | (Night) | |
Summoned By | Suspicious Looking Eye | |
Drops | ||
1-3 Corrupt Seeds | 100% | |
30-87 Demonite Ore | 100% | |
5-15 Lesser Healing Potions | 100% | |
20-49 Unholy Arrows | 100% | |
8 Hearts | 100% |
Contents |
The Eye of Cthulhu can be summoned by using a Suspicious Looking Eye (which can either be found in random chests or can be crafted from 6 Lenses at a Demon Altar) at night. Also, it can randomly summon itself with a 33% chance each night if the following criteria are met:
- At least one player in the game world has at least 200+ health.
- The Eye of Cthulhu has not already been defeated in the world.
While playing, the player may get the message, "You feel an evil presence watching you...", which means that the Eye will awaken soon. After a few minutes the message "The Eye of Cthulhu has awoken!" will appear and the boss will promptly start to attack the player. However, if "You feel an evil presence watching you..." and you aren't ready to fight the Eye of Cthulhu, you can opt out of fighting it by simply exiting and restarting the world or also restarting Terraria.
Disclaimer: For the purposes of this guide, it is assumed that the player is using a new character in a new world, and would therefore not have access to high-tier equipment, such as Molten Armor, a Fiery Greatsword, a Star Cannon, etc. Otherwise, this boss would go down in a matter of seconds.
The Eye of Cthulhu has two phases that it goes through as it does battle with the player. The first phase, a giant eye (shown to the left), has 18 attack power and 6 defense, while the 2nd phase, a giant eye with a gaping jaw in place of its lens (shown to the right), has a whopping thirty attack power, but only three defense.
Preparation is key when going up against what's likely to be your 1st boss (or for any other boss in this game). Since the Eye of Cthulhu can only summon itself if your max HP is 200 or more, you can delay its arrival by holding onto any Life Crystals that'll increase your max HP to 200 or more until you feel that you're ready. That way, you'll be able to wait until you can craft Golden Armor and a Gold Bow. However, if you're not patient enough to want to grind for golden-tier equipment, then you should at least have Iron Armor or better, an Iron Broadsword or better, and, most importantly, some sort of ranged weapon, such as Shuriken, Throwing Knives, or a bow (preferably Iron or better) with Flaming Arrows. Also, bring along any Lesser Healing Potions in case you need to heal. If possible, get glowing mushrooms for Healing Potions instead.
Another strategy would require the player to find an explosive weapon underground as soon as possible and have the Demolitionist spawn. Once the player had access to a steady supply of Bombs or Dynamite, and either a Featherfall Potion or a Hook they would then have to go to the Corruption and destroy a Shadow Orb as soon as possible in order to gain a Musket. Once the Arms Dealer arrived the player could then work out a way to obtain 5 gold and 35 silver for a Flintlock Pistol and 500 Musket Balls. One could use as low as copper armor for the Eye of Cthulhu provided they made sure to heal themselves properly before moving to phase two. As the EoC could almost be described as passive during phase one it would allow the player enough time to heal before moving on.
The following consumables may also be of some help:
- Ironskin Potion: This will increase your defense by 8 for five minutes, allowing you to take up to four less damage from the Eye of Cthulhu's attacks.
- Thorns Potion: For two minutes, enemies will take half of the damage that you take. This can make the battle go a bit quicker, though you'll probably want to try to avoid the Eye's attacks, especially during phase two, where they can do a whopping thirty damage. It can cause the Servants of Cthulhu to die instantly on contact with you, though you shouldn't let them touch you anyways, as they'll deal twenty-three damage.
- Archery Potion: For four minutes, the damage dealt by your bow & arrow increases by 20%, which will help decrease the time of the battle greatly.
- Regeneration Potion: For two minutes, your health regeneration is augmented, allowing you to recover more lost health in a faster period of time.
- If you have explored enough, and you are better with melee weapons in general, a Gravitation Potion with a silver or golden Broadsword may also be of use.
Weapons Analysis
- Shurikens: These weapons can be thrown rapidly and can penetrate through enemies, meaning that these can not only kill Servants of Cthulhu in one hit (thanks to their attack power of 10), but they'll also go on to damage the Eye itself. Although they only deal 4 damage to the Eye's 1st phase, due to their piercing mechanics, they'll often damage the Eye more than once, making them an ideal weapon. They're pretty easy to obtain as well, since not only are they commonly found in pots, but they can be purchased from the Merchant at any time for only 20 copper each. Throwing them straight in the iris of the Eye will hurt the servants as well.
- Throwing Knives: Although they are a bit harder to get than Shurikens (they're also common in pots, though the Merchant will also sell them during a Blood Moon for 50 copper each), they deal a bit more damage, and can likewise be thrown rapidly and penetrate enemies. They deal 6 damage to the Eye of Cthulhu's 1st phase, and can hit the Eye more than once per throw. However, if you're skilled (or lucky) enough to have access to Vile Powder (which is crafted with Vile Mushrooms from the Corruption), you can use that to upgrade your Throwing Knives into Poisoned Knives, which deal 7 damage to the Eye's 1st phase, and can even poison it, inflicting even more damage in the process.
- Bow & Arrow: Although you cannot fire a bow and arrow as rapidly as you can throw Shurikens or Throwing Knives, it's on here due to its potentially high damage output. A Golden Bow with Flaming Arrows deals 17 damage, which means that it'll deal 11 damage to the Eye's 1st phase. While Flaming Arrows cannot penetrate enemies like Shuriken or Throwing Knives can, it does have a chance of setting enemies on fire, damaging the Eye even further. On the other hand, a Golden Bow with Unholy Arrows (which are made out of normal arrows and Worm Teeth, which are dropped from Devourers) deals 19 damage (13 damage to the Eye's 1st phase), and can penetrate enemies like Shuriken and Throwing Knives can, though it'll travel too fast to damage the Eye multiple times.
- Musket: if you have Silver Bullets, this could be of use. Regular Musket Balls work as well, but you should have Golden or Silver Armor and Lesser Healing Potions or Healing Potions, as its very slow speed can make it difficult to do consistent damage. With Musket Balls it does 30 damage in the second phase, and 18 in the first.
- Rare Weapons: Most rare weapons you find in chests in the game will help you a lot. For example you can use an Enchanted Boomerang with your armor (Gold or better) and Healing Potions you should be able to defeat the eye easily.
Mobility in all directions (not just to the left or right) is important in avoiding the Eye of Cthulhu's attacks, and chances are that you won't have access to such items as Rocket Boots or Hermes Boots. Due to the player's limited jumping skills (only 6 blocks high, or 12 feet), it is strongly advised that you build a boss arena that consists of multiple rows of wooden platforms. (4 is a good number of floors for your arena to have.) Also, the arena must be reasonably wide enough to move around in comfortably. (At least 64 blocks wide is a good width.) Finally, the arena should have some tall walls to keep other enemies from entering the arena, though a ceiling isn't required. With no ceiling, Shurikens, Throwing Knives, and Arrows that are thrown upwards would fall back into the arena, and can still damage the Eye of Cthulhu during the descent.
Also remember to light the arena with torches, as the battle can only take place at nighttime.
The Battle Itself
The Eye of Cthulhu can only be summoned during night-time and will disappear without dropping any loot if the player does not kill it before daytime. Therefore, the best time to summon this monster would be soon after nightfall. That way, you'll have pretty much all night to defeat it.
Phase 1
The Eye of Cthulhu will try to hover high above the player and shoot out a Servant of Cthulhu every couple of seconds from the iris. The Servants of Cthulhu each have an attack of 12, but only 8 HP, which is low enough for them to die from one Shuriken. While the Eye is summoning Servants, you should be aiming for the pupil, as that's where the Servants will spawn from. If any stray Servants do get too close, then a Broadsword is useful for getting them out of your hair.
After four to six Servants of Cthulhu have been launched, the Eye of Cthulhu will start to dive towards the player three times. It has an attack power of 18, which can be damaging if care is not taken. Still, players should try to avoid these dive attacks whenever possible, changing to a higher or lower level if need be. Note that it's possible to lead the Eye's dive attacks by jumping before it attacks.
Phase 2
Once the Eye of Cthulhu reaches 1400 HP or below, it'll start to spin around violently, shedding its iris "covering" (and lowering its defense to 3) to reveal a jaw full of sharp teeth, and setting the stage for phase 2 of the battle. While this happens, it is recommended to damage it as much as you can, due to lack of movement and retaliation. While the Eye no longer spawns Servants of Cthulhu during this phase, it hovers closer to the player to ensure that its dive attacks (which now do 30 damage) are more accurate. It also attacks quicker, making it more difficult to lead its attacks.
However, while the Eye of Cthulhu's speed is usually faster than the player, its acceleration and deceleration is rather poor. A clever player can exploit this by running in one direction, causing the Eye to give chase, then immediately stopping and running in the other direction, causing the Eye to drift away as it struggles to keep up with the player.
- Demonite Ore 100%
- Unholy Arrows 100%
- Coins 100%
- Gold Coin
- Small Hearts
- Corrupt Seeds 100%
- If a player uses the Suspicious Looking Eye after he or she received "You feel an evil presence watching you..." message (provided the message was received at night) an Eye Of Cthulhu will spawn and shortly after another Eye Of Cthulhu will appear, thus leaving the player to fight two bosses at the same time.
- If the Eye of Cthulhu is hit by a falling star, it will take 1000 damage, minus its current phase armor.
- If you attempt to summon the Eye of Cthulhu while another Eye of Cthulhu is already present in the world, you will die instantly. Also, one of the Eye of Cthulhu's may remain after you respawn.
- A player using Hermes Boots may be able to out-run the Eye of Cthulhu.
- There is a glitch where if The Eye of Cthulhu is summoned during a Blood Moon using a Suspicious Looking Eye the Dryad may not spawn.
- Late in the game, The Eye if Cthulhu can be an easy source of gold coins, because it can be defeated easily (Endgame players can defeat him in mere seconds) and the Demonite dropped from can be sold for a lot of money, but make sure to smelt it into bars first, as they're worth more than the raw ore.
- The Eye of Cthulhu is named after the fictional extraterrestrial entity, Cthulhu, created by horror author H. P. Lovecraft.
- The correct pronunciation of Cthulhu has long been debated. KAH-THOO-LOO and CHA-THOO-LAH are two commonly argued pronunciations. In reality, Lovecraft intended the name to be unpronouncable, as the creature pre-dated the English language.
- In patch 1.0.3, during multiplayer, if you pulled out a Suspicious Looking Eye, an Eye of Cthulhu would spawn and your Suspicious Looking Eye would not be taken away.
- A boss resembling the Eye of Cthulhu, known as Monoculus, was introduced to the FPS game Team Fortress 2, around Halloween, 2011. Monoculus appeared as a large eyeball shooting smaller eyeball projectiles in a similar manner to the Eye of Cthulhu.
- The Merchant has claimed he occasionally feels an evil presence watching him, perhaps stating that not unlike Skeletron, his curse monster is the EoC. He also states that he hopes a 'scrawny little kid' like the player isn't the only thing standing between the NPCs and the Eye of Cthulhu.
Update Info
- Health dropped from 3,000 HP to 2,800 HP.
- Doesn't drop Heart Crystals anymore.
- Introduced.


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subset: commoncrawl


text:
CSIRO Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia
The catalogue includes all published rotation-powered pulsars, including those detected only at high energies. It also includes Anomalous X-ray Pulsars (AXPs) and Soft Gamma-ray Repeaters (SGRs) for which coherent pulsations have been detected. However, it excludes accretion-powered pulsars such as Her X-1 and the recently discovered X-ray millisecond pulsars, for example, SAX J1808.4-3658 (Wijnands & van der Klis, Nature, 394, 344, 1998).
The catalogue can be accessed in a number of different ways. The simplest is from a web interface ( http://www.atnf.csiro.au/research/pulsar/psrcat ) allowing listing of the most commonly used pulsar parameters, their uncertainties and reference information. Several options for tabular output format are provided. Currently, a total of 67 predefined parameters are available: see the parameter list in Appendix A of this help file. A facility is provided for plotting of parameter distributions, either as two-dimensional plots or as histograms. Zoom facilities and interactive identication of plotted points are provided. Custom parameters can be defined by combining parameters in expressions using mathematical operators and functions and these can be either listed or plotted. Finally, the sample of pulsars listed or plotted can be limited by logical conditions on parameters, pulsar name (including wild-card names) or distance from a nominated position. These facilities are described in more detail below and links are provided within the web interface to relevant documentation.
After creating a table or plot, accessing the help pages or reference list, use your browser Back funtion to return to the main catalogue page.
For professional astronomers, a more detailed web interface is available allowing access to parameters of specialist interest and use of custom databases which may be either merged with or used in place of the public database. The catalogue can also be accessed using a command-line interface on unix or linux systems. Contact the authors if you would like access to these facilities.
The purpose of this documentation is to provide a description of all the features available. A more basic tutorial is available to guide the user through the web interface (http://www.atnf.csiro.au/research/pulsar/psrcat/Tutorial/intro.html). We encourage you to send us as much feedback (both positive and negative) as possible about the catalogue, interfaces and documentation.
PLEASE NOTE: If you make use of the ATNF Pulsar Catalogue in a
publication, we request that you acknowledge the source of the
information by referencing the paper: Manchester, R. N., Hobbs,
G. B., Teoh, A. & Hobbs, M., Astron. J., 129, 1993-2006 (2005)
(astro-ph/0412641), which gives a full description of the catalogue, and
by quoting the web address
Where practicable, please list the original references for data
used. Reference lists for data in a given table, both in plain text
and in .bbl format, are available from links at the bottom of the table
Microsoft Internet Explorer 5 |
lynx, version 2.8.3 |
Clicking on the pulsar name gives links to other databases which may
contain information about this pulsar. Clicking on a parameter name brings
up the list of parameter descriptions (Appendix A) in which the selected
parameter is highlighted in red.
Custom variables are functions of the predefined variables. Up to
four custom variables (C1, C2, C3 and C4) may be defined. The definition
is provided in the text box. Valid expressions for this definition
are given in section 4 of this documentation.
This custom variable can subsequently be used in sorting,
or plotted output. If the check-box to the left of the custom variable
label is checked then this variable will be listed in any tabular output
(in exponential form to 6 decimal places). For example, a new variable
(C1) can be defined to equal the square root of the period multiplied by
its derivative -- enter into one of the C1, C2, C3 or C4 text boxes sqrt(p0*p1)
click on the check-box to the left of the text:
Often the user will require results from only a selection of pulsars
in the catalogue. Filtering can be carried out on the pulsars' parameters
(described in this section), by the pulsars' names
(section 3.4) or by their position (section
3.5). The conditional expression can be any valid
expression (section 4) with the following conditional
== | Equality | != | Inequality test |
< | Less than | ! | Logical NOT |
<= | Less than or equal to | && | Logical AND |
> | Greater than | || | Logical OR |
>= | Greater than or equal to |
along with the following functions:
exist(pmtot) && exist(pb)
exist(pmra) && error(pmra) < 20
or to select all pulsars which do not emit at radio wavelengths:
or to select all pulsars which do not emit at radio wavelengths:
assoc(snr) will select all pulsars with SNR associations.
will return pulsars within the required range. The coordinate type can be raj, rajd, gl or elong.
It is possible to supply right ascensions in hours, minutes and seconds and declinations in degrees, minutes and seconds as follows:
raj > h19:33 && decj < d-30:00
(note, the use of an 'h' to indicate hours,minutes and seconds and 'd' for degrees). This can also be used within the range function:
This format requires a colon (i.e. hours/degrees and minutes must be entered; the use of seconds is optional). The functions hms() and dms() may be used to convert to degrees. For example,
raj > hms(19:33) && decj < dms(-30:25)
It is possible to select pulsars that have been individually entered into the "Pulsar names" box. For example:
would produce a table including only the pulsars B0329+54, B1933+16
and J2346-0609. The pulsar names can be separated by a new line,
comma, tab character or spaces. It is advisable to include the `B'
or `J' in front of the pulsar name; if not both the pulsar B1950
and J2000 names will be searched for a match to the entered name.
The name may include the wildcard characters `*' and `?'. For example,
b1933+1? will match PSRs B1933+16, B1933+17 and B1933+15 whereas j004*+*
will match PSRs J0040+5716 and J0048+3412.
The user may wish to obtain all (or a large amount of) the information
stored for a few pulsars. This is possible, but not practical, using
the standard table forms. It is, therefore, possible to type the
names of the pulsars of interest in the `Pulsar names' area and then to
select "Get Ephemeris". Three output formats are available. Short
format provides all the pulsar parameters stored in the catalogue that
are understood by the TEMPO
[external link] pulsar timing package (most of the observed astrometric
and rotational parameters, but no derived parameters). Long
format provides all the information obtainable from the data stored in
the catalogue (all observed, survey and derived parameters) and the Selected
format uses the parameter selections made in the `predefined variables'
section to define which parameters to display. Examples are shown below.
Short format
Long format
Equatorial coordinates can be entered using white spaces or colons, for example "19:33:00" is treated in the same manner as "19 33 00", "19 33" and "19:33". It is sometimes necessary to know the angular distance between each pulsar and the central coordinate. Selecting `Show pulsar's distance from centre of this region' will provide a new column in the tabular output giving this angular distance in degrees.
The final table can take five different forms: `short', `short
with errors', `long with last digit errors', `long with errors' or
`publication quality', with 'long with last digit errors' as
default. The short form is used to provide a condensed summary of the
pulsar parameters; periods are given to six decimal places, dispersion
measures to two decimal places etc. It is expected that this
format will be used for producing tables that can be entered directly
into, for instance, plotting packages where the full measured
precision is not required. The short format with errors produces
a similar table, but provides uncertainties on the parameters that
have corresponding errors. The actual value of the parameter is
given to the same number of decimal places as the "short"
format. The uncertainty is given in an exponent format to one
decimal place. The long formats provides the parameters to their
measured precision, their uncertainties and references. From the
web interface it is possible to click on a reference label to obtain
the full bibliographic reference (see section
8). The uncertainty is given as an integer corresponding to the
uncertainty in the last significant figure in the value. For
example, "1.2 2" can be written as "1.2 +/-
0.2". The `publication quality' format gives the parameters to
full precision with corresponding uncertainties given in
parenthesis. For example, 3.4(5) could also have been written as
3.4 +/- 0.5. The bibliographic references are included as a
separate column on the right hand side of the table. The example
below shows the table produced with the different output formats for
the three pulsars with periods less than two milliseconds:
short: | |
short with errors: | |
long with last digit errors: | |
publication: |
Selecting `No header' will produce a table with no header information at the top and with no spaces between groups of five pulsars. If a parameter has been selected, but does not exist in the catalogue (for example, not all pulsars have had their proper motions measured) then the table will contain a `null value'. By default, this null value is set to a '*'. However, the user may enter any string into the Null Value text box to modify this output. For example, the user could enter: "-999.999" or "no value".
Tabular output may be copied to a local disk using the browser 'Save
As' function with Text format. Netscape provides a method of bypassing
the screen display: pressing Shift and the Table button together will copy
the output directly to the local disk. Alternatively, Select, Copy and
Paste functions may be used. Graphical output may be copied to a local
disk using a screen capture program such as xv.
It is possible to display functions of the pulsar parameters as
a graph or as a histogram. For a normal (x-y) graph, the values
to plot are defined as regular expressions (see examples in section
4) and the axes of the graph can be displayed linearly or logarithmically.
The expressions may contain custom-defined variables. In the following
example the user is plotting rotational periods against period derivatives
on a logarithmic scale:
Binary pulsars are indicated in blue, AXP/SGRs are green, high energy pulsars are purple and the remainder in red. It is possible to select a region on the plot using the mouse cursor, clicking and releasing the LH button to define the region. The names of the pulsars lying within these region are displayed to the right of the graph. Clicking on a pulsar name will put cross-hairs on the pulsar's position on the graph. The selected region can be expanded by clicked on `Zoom in' and the graph reverted to its original form by selecting `Reset Plot'.
Histograms can be produced by only entering an expression into the x-axis
text-box. For example to form a histogram of the logarithm of the
rotational periods, type P0 in the x-axis box and select a logarithmic
scale and then click on .
This will give the following output:
The blue colour represents binary pulsars, green AXP and SGRs and purple high energy pulsars. Clicking on any bar will provide a listing of all the pulsars that lie within that bin of the histogram. The number of bins can be increased or decreased by typing the required number of bins under the Number of bins heading or by clicking on the left and right arrows to decrement or increment the number of bins respectively.
+ | Addition |
- | Subtraction |
* | Multiplication |
/ | Division |
** | Raise to the power |
= | assignment |
acos | inverse cosine | sin | sine of angle in radians |
asin | inverse sine | sind | sine of angle in degrees |
atan | inverse tangent | sinh | hyperbolic sine |
atan2 | inverse tangent | sqr | square |
cos | cosine of angle in radians | sqrt | square root |
cosd | cosine of angle in degrees | tan | tan of angle in radians |
cosh | hyperbolic cosine | tand | tan of angle in degrees |
exp | exponential | tanh | hyperbolic tangent |
ln | log (base 2) | fabs | absolute value |
log | log (base 10) | fmod | modulus (two arguments) |
log10 | log(base 10) |
Each function (except fmod) takes only one variable or expression which
should be typed immediately after the function name and enclosed in parentheses.
The table below lists the major pulsar surveys. The category 'misc'
lists pulsars discovered in other (more limited) searches.
Reference Keys |
ar1 | Arecibo Survey 1 | ht75 | 4 | 49 | 41 |
ar2 | Arecibo Survey 2 | sstd86 | 400 | 24 | 6 |
ar3 | Arecibo Survey 3 | nft95 | 2000 | 61 | 24 |
ar4 | Arecibo Survey 4 | wol90a,cnt93,fwc93,nft93,tdk+93,cam95a,
fcwa95,cnt96,cnst96,rtj+96,snt97,lwf+04, lxf+05 |
20000 | 120 | 74 |
palfa | Arecibo Multibeam Survey | cfl+06,lsf+06,hng+08,dcm+09,kac+10,kla+11,dfc+12,csl+12 | 2000000 | 55 | 26 |
FermiBlind | Fermi Gamma-ray Observatory blind survey | aaa+09c,sdz+10,rkp+11,awd+12,pga+12,pga+12a | 4000000 | 37 | 37 |
FermiAssoc | Searches of unidentified Fermi gamma-ray sources | rrc+11,kjr+11,ckr+12,gfc+12,kcj+12,rap+12,bgc+13 | 20000000 | 39 | 39 |
gb1 | Green Bank Northern Hemisphere survey | dth78 | 20 | 50 | 31 |
gb2 | Princeton-NRAO survey | dtws85 | 40 | 83 | 34 |
gb3 | Green Bank short-period survey | stwd85 | 200 | 86 | 20 |
gb4 | Green Bank fast pulsar survey | nst96,snt97 | 10000 | 83 | 5 |
gb350 | Green Bank 350 MHz drift-scan survey | hrk+08,rsm+12,blr+13,lbr+13 | 40000000 | 59 | 58 |
htru | Parkes high time resolution survey | kjv+10,lbb+10,bbb+11a,kjb+12,bbb+12 | 10000000 | 813 | 86 |
jb1 | Jodrell A survey | dls77 | 2 | 51 | 37 |
jb2 | Jodrell B survey | cl86 | 100 | 62 | 42 |
mol1 | 1st Molonglo survey | vl70 | 1 | 34 | 31 |
mol2 | 2nd Molonglo Survey | mlt+78 | 10 | 224 | 155 |
pks1 | Parkes 20-cm survey | jlm+92 | 1000 | 100 | 46 |
pks70 | Parkes Southern Sky survey | mld+96,lml+98 | 4000 | 298 | 101 |
pkshl | Parkes high-latitude multibeam pulsar survey | bdp+03,lbk+04,bjd+06 | 1000000 | 42 | 18 |
pksgc | Parkes globular cluster survey | mld+90,mlr+91,rlm+95,clf+00,dlm+01,dfp+02,pdm+03,fre08 | 200000 | - | 33 |
pksmb | Parkes multibeam pulsar survey | mlc+01,mhl+02,kbm+03,hfs+04,fsk+04,lfl+06,kle+09,kel+09,mlb+12,kek+13,elkl13 | 40000 | 1114 | 825 |
pkssw | Parkes-Swinburne multibeam survey | ebvb01,jbv+03,jac04a,jbo+09,bb10 | 100000 | 243 | 108 |
pkspa | Parkes Perseus Arm multibeam survey | bkl+13 | 100000000 | 15 | 15 |
misc | -- | 400000 | - | 306 |
The Galactocentric coordinate system (XX, YY, ZZ) is right-handed
with the Sun at (0.0, 8.5 kpc, 0.0) and the ZZ axis directed toward
the north Galactic pole.
the `Name' and `Email' boxes are not compulsory, but should be included
if you require a reply to your comment.
The catalogue database will be upgraded both in response to user
feedback and to include data from recent publications.
Type the name of your database file in the box, using the Browse
function to find the correct directory if necessary. Then hit the
"Upload to ATNF" button and the file will be transferred to an ATNF
disk. A message will report whether or not the upload was successful.
This operation may be repeated to transfer multiple files.
To merge the file(s) with the public database, with precedence given
to later files in the list, click on the Merge button.
Then you may create a table or plot as usual by selecting parameters and
clicking the appropriate button.
If you click the "Delete file immediately after use" button, the
file(s) will be deleted from the ATNF disk after the next operation
(table or plot). Otherwise, they will be left there
indefinitely. However, we
reserve the right to delete files more than one year old.
The current catalogue database and the PSRCAT source code may
be downloaded by clicking on the "Download" link at the top of the
Catalogue webpage.
PSRCAT is free software: you can redistribute it and/or modify
it under the terms of the GNU General Public License as published by
the Free Software Foundation, either version 3 of the License, or
(at your option) any later version.
PSRCAT is distributed in the hope that it will be useful,
but WITHOUT ANY WARRANTY; without even the implied warranty of
MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the
GNU General Public License for more details.
PSRCAT makes use of "evaluateExpression: A Simple Expression Evaluator".
Copyright (c) 1996 - 1999 Parsifal Software, All Rights Reserved.
9.1 Custom databases
We regret that, because of hacking problems, the upload facility has been disabled.
In 'Expert' mode, the user is able to upload to the ATNF system one or
more custom databases to be displayed by the web interface. This
facility is also available in the command-line interface version of
psrcat. These databases may either replace the public database or be
merged with it.
9.1.1 Uploading a custom database
At the bottom of the page, there is a section called "Attach your own
Catalogue" as shown below:
9.1.2 Using a custom database
Type the name of your file in the box immediately above, labelled
"File Name:" as shown in the example below. Multiple file names may be
entered, separated by commas or spaces.
10. Downloading the Catalogue
The web interface was designed and constructed by Albert
Teoh, during his tenure as a Summer Vacation Scholar at the ATNF,
This work has made extensive use of NASA's
Astrophysics Data System and the
Google search engine.
The original database was compiled with the invaluable assistance of
Maryam Hobbs during her term as a Research Assistant in the ATNF
Parkes Pulsar Timing Array (PPTA) group (10/2003 - 4/2005). Since then
this work has been continued by Diana Londish (8/2005 - 10/2006),
Lucyna Kedziora-Chudczer (11/2006 - 6/2009), Ankur Chaudhary (9/2009 -
9/2012) and Lawrence Toomey (12/2012 - present).
We thank W. Becker for a pre-publication copy of "X-ray Emission from
Pulsars and Neutron Stars", in "Neutron Stars and Pulsars",
Astrophys. Space Sci. Library 357 (2008), Thomas Tauris and
Paulo Freire for assistance with compiling the list of binary
companion types and relevant references (see Tauris, Langer and
Kramer, 2012, MNRAS, 425, 1601) and Meng Yu for updates to the glitch
table. We acknowledge the use of Paulo Freire's website
Pulsars in Globular Clusters and the
McGill AXP/SGR Online Catalog
which have provided valuable cross-checks and, in some cases, otherwise
unpublished data. Finally, we thank our colleagues for their many
comments and suggestions which have helped to improve both the
database and the means of accessing it.
Appendix A: The Pulsar
Name: Pulsar name. The B name if exists, otherwise the J name.
JName: Pulsar name based on J2000 coordinates
RAJ: Right ascension (J2000) (hh:mm:ss.s)
DecJ: Declination (J2000) (+dd:mm:ss)
PMRA: Proper motion in the right ascension direction (mas/yr)
PMDec: Proper motion in declination (mas/yr)
PX: Annual parallax (mas)
PosEpoch: Epoch at which the position is measured (MJD)
ELong: Ecliptic longitude (degrees)
ELat: Ecliptic latitude (degrees)
PMElong: Proper motion in the ecliptic longitude direction (mas/yr)
PMElat: Proper motion in ecliptic latitude (mas/yr)
GL: Galactic longitude (degrees)
GB: Galactic latitude (degrees)
RAJD: Right ascension (J2000) (degrees)
DecJD: Declination (J2000) (degrees)
Bname: Pulsar Besselian name
PML: Proper motion in Galactic longitude (mas/yr)
PMB: Proper motion in Galactic latitude (mas/yr)
Timing solution and profile parameters:
P0: Barycentric period of the pulsar (s)
P1: Time derivative of barcycentric period (dimensionless)
F0: Barycentric rotation frequency (Hz)
F1: Time derivative of barycentric rotation frequency (s-2)
F2: Second time derivative of barycentric rotation frequency (s-3)
F3: Third time derivative of barycentric rotation frequency (s-4)
PEpoch: Epoch of period or frequency (MJD)
DM: Dispersion measure (cm-3 pc)
DM1: First time derivative of dispersion measure (cm-3 pc yr-1)
RM: Rotation measure (rad m-2)
W50: Width of pulse at 50% of peak (ms). Note, pulse widths are a function of both observing frequency and
observational time resolution,so quoted widths are indicative only. Refer to the original reference for details.
W10: Width of pulse at 10% (ms). Note the comments above for W50.
Tau_sc: Temporal broadening of pulses at 1 GHz due to interestellar scattering (s)
S400: Mean flux density at 400 MHz (mJy)
S1400: Mean flux density at 1400 MHz (mJy)
S2000: Mean flux density at 2000 MHz (mJy)
F4: Fourth time derivative of barycentric rotation frequency (s^-5)
F5: Fifth time derivative of barycentric rotation frequency (s^-6)
F6: Sixth time derivative of barycentric rotation frequency (s^-7)
F7: Seventh time derivative of barycentric rotation frequency (s^-8)
F8: Eighth time derivative of barycentric rotation frequency (s^-9)
F9: Ninth time derivative of barycentric rotation frequency (s^-10)
FA: Tenth time derivative of barycentric rotation frequency (s^-11)
FB: Eleventh time derivative of barycentric rotation frequency (s^-12)
FC: Twelfth time derivative of barycentric rotation frequency (s^-13)
DM2: Second time derivative of dispersion measure (cm-3pc yr-2)
DM3: Third time derivative of dispersion measure (cm-3pc yr-3)
DM4: Fourth time derivative of dispersion measure (cm-3pc yr-4)
DM5: Fifth time derivative of dispersion measure (cm-3pc yr-5)
DM6: Sixth time derivative of dispersion measure (cm-3pc yr-6)
DM7: Seventh time derivative of dispersion measure (cm-3pc yr-7)
DM8: Eighth time derivative of dispersion measure (cm-3pc yr-8)
DM9: Ninth time derivative of dispersion measure (cm-3pc yr-9)
S600: Flux at 600 MHz (mJy)
S700: Flux at 700 MHz (mJy)
S800: Flux at 800 MHz (mJy)
S900: Flux at 900 MHz (mJy)
S1600: Flux at 1600 MHz (mJy)
S3000: Flux at 3000 MHz (mJy)
SPINDX: Radio spectral index
Binary system parameters:
Binary: Binary model (usually one of several recognised by the pulsar timing programs TEMPO or TEMPO2
T0: Epoch of periastron (MJD)
PB: Binary period of pulsar (days)
A1: Projected semi-major axis of orbit (lt s)
OM: Longitude of periastron (degrees)
ECC: Eccentricity
TASC: Epoch of ascending node(MJD) - ELL1 binary model
Eps1: Ecc x sin(OM) - ELL1 binary model
Eps2: Ecc x cos(OM) - ELL1 binary model
MinMass: Minimum companion mass assuming i=90 degrees and neutron star mass is 1.35 Mo
MedMass: Median companion mass assuming i=60 degrees
BinComp: Companion type
OMDOT: Periastron advance (deg/yr)
PBDOT: 1st time derivative of binary period
A1DOT: Rate of change of projected semi-major axis
ECCDOT: Rate of change of eccentricity
GAMMA: Post-Keplerian gamma term (s)
T0_2: Epoch of periastron [2nd orbit] (MJD)
PB_2: Binary period of pulsar [2nd orbit] (days)
A1_2: Projected semi-major axis of orbit [2nd orbit] (s)
OM_2: Longitude of periastron [2nd orbit] (deg)
OMDOT_2: Periastron advance [2nd orbit] (deg/yr)
ECC_2: Eccentricity [2nd orbit]
PBDOT_2: 1st time derivative of binary period [2nd orbit]
T0_3: Epoch of periastron [3rd orbit] (MJD)
PB_3: Binary period of pulsar [3rd orbit] (days)
A1_3: Projected semi-major axis of orbit [3rd orbit] (s)
OM_3: Longitude of periastron [3rd orbit] (deg)
OMDOT_3: Periastron advance [3rd orbit] (deg/yr)
ECC_3: Eccentricity [3rd orbit]
PBDOT_3: 1st time derivative of binary period [3rd orbit]
PPNGAMMA: PPN parameter gamma (s)
SINI: Sine of inclination angle
SINI_2: Sine of inclination angle [2nd orbit]
SINI_3: Sine of inclination angle [3rd orbit]
MTOT: Total system mass (solar masses)
M2: Companion mass (solar masses)
M2_2: Companion mass [2nd orbit] (solar masses)
M2_3: Companion mass [3rd orbit] (solar masses)
DTHETA: Relativistic deformation of the orbit
XOMDOT: Rate of periastron advance minus GR prediction (deg/yr)
XPBDOT: Rate of change of orbital period minus GR prediction
DR: Relativistic deformation of the orbit (not fitted)
A0: Aberration parameter A0 (s, not fitted)
B0: Aberration parameter B0 (s, not fitted)
BP: Tensor multi-scalar parameter beta-prime (not fitted)
BPP: Tensor multi-scalar parameter beta-prime-prime (not fitted)
MASSFN: The pulsar mass function (solar mass)
UPRMASS: 90% confidence upper companion mass limit, i=26deg (solar mass)
MINOMDOT: Minimum omega dot, assuming sin i = 1 and M_ns = 1.4Mo (deg/yr)
Distance parameters:
Dist: Best estimate of the pulsar distance using the tc93 DM-based distance as default (kpc)
Dist_DM: Distance based on the tc93 electron density model.
In `LONG' or `PUBLICATION QUALITY' modes, lower limits from the distance model are preceded by a `+' sign.
DMsinb: DM x sin(b) (cm-3 pc)
ZZ: Distance from the Galactic plane, based on Dist
XX: X-Distance in X-Y-Z Galactic coordinate system (kpc)
YY: Y-Distance in X-Y-Z Galactic coordinate system (kpc)
Dist_DM1: Distance based on NE2001 model (kpc)
Dist1: Best estimate of the pulsar distance using the NE2001 DM-based distance as default (kpc)
Dist_A: Independent distance estimate - takes precedence over other distance estimates for DIST and DIST1 (kpc)
Dist_AMN: Lower limit on independent distance estimate (kpc)
Dist_AMX: Upper limit on independent distance estimate (kpc)
Associations and survey parameters:
Assoc: Names of other objects, e.g., supernova remnant, globular cluster or gamma-ray source
associated with the pulsar
Survey: Surveys that detected the pulsar (discovery survey first). Click here for currently defined surveys.
OSurvey: Surveys that detected the pulsar encoded as bits in integer
Date: Date of discovery publication.
Type: Type codes for the pulsar. Click here for available types.
NGlt: Number of glitches observed for the pulsar
TRES: RMS timing residual (microsec)
NTOA: Number of TOAs in timing fit
START: Epoch of start of fit (MJD)
FINISH: Epoch of end of fit (MJD)
CLK: Terrestrial time standard
EPHEM: Solar system ephemeris
TZRMJD: Reference TOA (MJD)
TZRFRQ: Frequency of reference TOA (MHz)
TZRSITE: One-letter observatory code for reference TOA
TDMP: Ideal subintegration time for pulsar (s)
TDMPMIN: Minimum subintegration time for pulsar (s)
NSPAN: Minutes for polyco span
NCOEF: Number of coefficients in polyco
NBIN: Number of bins in the profile
NSUB: Number of subbands to store
GLEP: Epoch of glitch
GLPH: Phase increment at glitch
GLF0: Permanent pulse frequency increment at glitch
GLFI: Permanent frequency derivative increment at glitch
GLF0D: Decaying frequency increment at glitch
GLTD: Time constant for decaying frequency increment
Derived parameters:
R_Lum: Radio luminosity at 400 MHz (mJy kpc2)
R_Lum14: Radio luminosity at 1400 MHz (mJy kpc2)
Age: Spin down age (yr) []
BSurf: Surface magnetic flux density (Gauss) []
Edot: Spin down energy loss rate (ergs/s)
Edotd2: Energy flux at the Sun (ergs/kpc2/s)
PMTot: Total proper motion (mas/yr)
VTrans: Transverse velocity - based on DIST (km/s)
P1_i: Period derivative corrected for proper motion effect
Age_i: Spin down age from P1_i (yr)
BSurf_i: Surface magnetic dipole from P1_i (gauss)
Edot_i: Spin down energy loss rate from P1_i (ergs/s)
B_LC: Magnetic field at light cylinder
User Parameters
PAR1: A non-standard parameter entered by the user
PAR2: A non-standard parameter entered by the user
PAR3: A non-standard parameter entered by the user
PAR4: A non-standard parameter entered by the user
AXP Anomalous X-ray Pulsar or Soft Gamma-ray Repeater with detected pulsations BINARY Pulsar has one or more binary companions HE Spin-powered pulsar with pulsed emission from radio to infrared or higher frequencies NRAD Spin-powered pulsar with pulsed emission only at infrared or higher frequencies RADIO Pulsars with pulsed emission in the radio band RRAT Pulsars with intermittently pulsed radio emission XINS Isolated neutron stars with pulsed thermal X-ray emission but no detectable radio emission
MS Main-sequence star NS Neutron star CO CO or ONeMg White Dwarf He Helium White Dwarf UL Ultra-light companion or planet (mass < 0.08 solar masses) Note: If there is more than one companion, "T" (for Triple) is appended to the companion type. The innermost companion determines the type.


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Lanzer, on 14 February 2012 - 04:21 PM, said:
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EDIT: Also, the cover may be new but none of the art on the cover is.


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Bouncy Castle wrote:Buildings collapse into a hole in China.
chillicamper wrote::shock: Imagine coming home from work to find whats left of your house down a huge hole.
Bouncy Castle wrote:Father of boy killed in school massacre heckled by pro-gun activists.
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Bouncy Castle wrote:Amazingly brave lady, on the same subject.
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By: Amanda Campbell
Updated: March 2, 2011
Your dishwasher should always be plugged into a grounded outlet. DO NOT use an extension cord.
If hot water has not been used in your house for more than two weeks or longer, open all the hot water faucets and allow them to run for several minutes before using your dishwasher or any other electrical appliance connected to the hot water heater. When you are doing this, be sure NOT to smoke or light any flame while the faucets are running as hydrogen gas which is flammable and explosive may have built up in the water heater and hot water pipes.
To help keep your dishwasher free of stains all you need is some powdered drink crystals. Use three to four ounces of the powdered drink crystals (orange or lemon work well). Be sure to read the back of the package to make sure there is citric acid in the crystals, it is the citric acid that does all the work. Place the powder in the soap dispenser. DO NOT put regular dishwashing detergent in the soap containers. Also make sure the dishwasher is empty when you run it with the powdered drink crystals. This will help you keep the inside of the dishwasher free of stains.
If you have hard water and need to remove the mineral build up you can try using white vinegar�but check the owner�s manual first to make sure the make and model will tolerate the vinegar. Then start your dishwasher on its regular cycle (be sure the dishwasher is empty). When the bottom of the dishwasher begins to fill with water open the door and pour two cups of vinegar on the floor of the dishwasher and close the door.
To make sure the water temperature is hot enough to clean your dishes properly go to the sink nearest the dishwasher. Turn on the hot water and let it run until it is as hot as possible. Place a meat thermometer in the running water to make sure the temperature is at least 140 degrees. If your hot water is not hot enough turn up the heat on your hot water heater or try insulating the pipes that run from the heater to the dishwasher.
If the outside of your dishwasher is white and you want to get rid of yellowing stains try mixing together � cup of bleach, � cup of baking soda and 4 cups of warm water. Apply this mixture with a sponge and let it set for about ten minutes then rinse and dry thoroughly, this will work on other white appliances as well.
Do tipped glasses half full of water drive you crazy when you try to unload the dishwasher? Try to �catch� your dishwasher when it is between the wash cycle and the dry cycle. Open the door, drain the dishes and the pools of water from glasses and cups and then close the dishwasher and allow it to finish its regular cycle. Your dishes should be completely dry and ready to be put away when the dry cycle is complete. Or try this, run your dishwasher at the end of the day. In the morning drain the dishes and then reset the dishwasher to run on the dry cycle for a few minutes.
A dishwasher can clean more than just dishes. Many figurines, knick-knacks, baby toys and some of your shelves and bins from the refrigerator are safe to run through the dishwasher and come out sparkling clean. Also, to disinfect your sponges try running them through the dishwasher in the top rack.
These quick tips will help you keep your dishwasher clean as well as your dishes.


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2013 Volkswagen Golf Bluemotion and GTI introduced at Paris motor show
Seventh-generation VW Golf shows off with concept version of its hot-hatch GTI brother
We learned the details on the seventh-generation 2013 Volkswagen Golf earlier this September, but at the Paris auto show the company announced more info on the BlueMotion and GTI versions.
The new VW GTI will sport 217 hp—10 more ponies than last year—from the same 2.0-liter turbocharged direct-injection gasoline engine. Torque grows to 258 lb-ft; that's as much as the Golf R we drove back in July.
VW will also offer a performance pack, boosting output to 227 hp. The GTI will make the 0-to-60 sprint in 6.6 seconds, with a top speed of 153 mph.
In addition to upping the power, the performance pack also comes with upgraded front brake discs and a limited slip set-up that reduces torque steer. A six-speed manual and a six-speed dual-clutch transmission are both available.
The new Volkswagen GTI also gets a variable ratio steering system, which reduces input when moving at slow speeds and parking.
Also at the show, VW revealed the 2014 Golf BlueMotion, which gets 88.3 mpg on the European test cycle. Fuel consumption is down 15 percent from the last generation, but capacity is up and the tank now holds 14.5 gallons.
The BlueMotion has lost weight—57 pounds in the running gear and 81 pounds in the body. It also uses low rolling resistance tires with higher air pressure, longer gear ratios and battery regeneration.
The BlueMotion gets a 1.6-liter turbo-diesel engine, making 108 hp and 184 lb-ft of torque.
The BlueMotion will launch in the United Kingdom in 2013, as will the GTI.
The 2012 Paris motor show, or as it is officially known – Mondail de l'Automobile – will take place Sept. 27 through Oct. 14, 2012. It occurs every two years alternating with the Frankfurt motor show in Germany. The Paris motor show is a spotlight for the latest in design, but automakers will also be showing off their latest concept cars, green cars and supercars.
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